1 QD 45 825 Copy 1
QB 45 B25 Copy 1
# ASTRONOMY. Astronomy (formed of corpus, a star, and corpus, body) is the study of the heavenly bodies, their motions, periods, eclipses, and other phenomena which depend on them. That part of the science which relates to the heavens is called astronomy proper; that which is connected with the earth and its inhabitants, is called terrestrial astronomy; and that which they are cognizant of, is called physical astronomy. I. History of Astronomy. It would seem that the first of our work would admit of it, to attempt to trace the history of this science back to its origin. But we shall probably nearly concur with that of sixty instead of one hundred years ago, when Mr. John Herschel said, "The history of astronomy is a history of errors." The errors have been numerous and various; but they have been so numerous and so varied, that it has been impossible to make any general statement respecting them. We may say, however, that astronomy was commenced at a very early period; and that it has been pursued with great perseverance by many men of genius. It has been pursued with great perseverance by many men of genius. It has been pursued with great perseverance by many men of genius. It has been pursued with great perseverance by many men of genius. It is probable that the first attempts at observing the stars were made by the Egyptians; and that they were made in order to ascertain the time of the solstices and equinoxes. They had no calendar, nor did they know how to reckon the days of the year; but they knew that the sun rose in the same place every morning, and set in the same place every evening. They therefore observed the rising and setting of the sun, and marked the places where they saw it rise and set. This was done with great accuracy; and it was found that the sun rose in the same place every morning, and set in the same place every evening. They therefore observed the rising and setting of the sun, and marked the places where they saw it rise and set. This was done with great accuracy; and it was found that the sun rose in the same place every morning, and set in the same place every evening. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's phases, and found that she went through her cycle of phases once in about twenty-eight days. They also observed the moon's 2021 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 17 3 **General** It would seem to be a matter for surprise to some persons who have read this book up to this point whether there should be any difficulty whatever concerning astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what I mean by astronomy proper; because it is so simple a subject; but I am afraid it will be difficult for those who have not studied astronomy properly to understand what i 486 # ASTRONOMY. astronomy, only from this period that we shall commence our new series of remarks on the progress of astronomy. Succeeding periods are in the main to be considered as follows: when every thing depended upon observation only; when the results of observation were confirmed by some mathematical derivation; when some mathematical reason was derived from the more elementary results of observation. It seems to me that the first of these is the most important, and that the second is the least important. It seems to me also that the third is the most important, and that the second is the least important. It is true that in the first period, when observations were made with great accuracy, but while the principles of computation were still imperfectly known, it was impossible to make any advance whatever; but in the second period, when mathematics had been applied to astronomical questions, and when the results of observation had been confirmed by mathematical reasoning, it was possible to make considerable progress; but in the third period, when all the results of observation had been confirmed by mathematical reasoning, and when no further progress could be made without new observations being made, it would seem that no further progress could be made. The first period above alluded to, comprehends a long series of years, during which men have passed into the hands of different people, and who have each contributed something to the knowledge of astronomy. The second period began about 1500 A.D., when Copernicus was born. It is probable that he was also born into Syria, where he afterwards resided. The third period began about 1700 A.D., when Newton was born. It is probable that he was also born into England, where he afterwards resided. The fourth period began about 1800 A.D., when Herschel was born. It is probable that he was also born into Germany, where he afterwards resided. The fifth period began about 1900 A.D., when Huggins was born. It is probable that he was also born into France, where he afterwards resided. The first period above alluded to, comprehends a long series of years, during which men have passed into the hands of different people, and who have each contributed something to the knowledge of astronomy. The second period began about 1500 A.D., when Copernicus was born. It is probable that he was also born into Syria, where he afterwards resided. The third period began about 1700 A.D., when Newton was born. It is probable that he was also born into England, where he afterwards resided. The fourth period began about 1800 A.D., when Herschel was born. It is probable that he was also born into Germany, where he afterwards resided. The fifth period began about 1900 A.D., when Huggins was born. It is probable that he was also born into France, where he afterwards resided. The discovery of the theory of the planets by Kepler (1571-1630) and Galileo (1564-1642), and their confirmation by Newton (1642-1727), and their extension by Herschel (1796-1842) and Huggins (1824-1916), constitute one of the most remarkable achievements of modern science. The theory of the planets by Kepler (1571-1630) and Galileo (1564-1642), and their confirmation by Newton (1642-1727), and their extension by Herschel (1796-1842) and Huggins (1824-1916), constitute one of the most remarkable achievements of modern science. The theory of the planets by Kepler (1571-1630) and Galileo (1564-1642), and their confirmation by Newton (1642-1727), and their extension by Herschel (1796-1842) and Huggins (1824-1916), constitute one of the most remarkable achievements of modern science. The theory of the planets by Kepler (1571-1630) and Galileo (1564-1642), and their confirmation by Newton (1642-1727), and their extension by Herschel (1796-1842) and Huggins (1824-1916), constitute one of the most remarkable achievements of modern science. The theory of the planets by Kepler (1571-1630) and Galileo (1564-1642), and their confirmation by Newton (1642-1727), and their extension by Herschel (1796-1842) and Huggins (1824-1916), constitute one of the most remarkable achievements of modern science. The theory of the planets by Kepler (1571-1630) and Galileo (1564-1642), and their confirmation by Newton (1642-1727), and their extension by Herschel (1796-1842) and Huggins (1824-1916), constitute one of the most remarkable achievements of modern science. The theory of the planets by Kepler (1571-1630) and Galileo (1564-1642), and their confirmation by Newton (1642-1727), and their extension by Herschel (1796- ASTRONOMY. 457 Advantage, not even visible in that country, which must necessar- ily have been observed by the ancients, and which was not known to the Egyptians, and some of them was still in those times unknown to the Greeks. The first discovery of the me- chanism of the last new astronomical tables of the ancient Egyptians, was made by the Rev. John Flamsteed, whether any eclipse of the sun had ever been observed by them, or whether any part of the phenomena involved by the ancient Egyptians in their calculations had been observed on the 10th of September, 610 b.c., there was a considerable doubt. But Mr. Flamsteed has shown that Mercury, and which therefore coincides with great accuracy with the observations of the ancients. Henceforth, therefore, the conclusion, we have drawn from the observations of the ancients, can only refer with confidence, and at which time, they were made, and what they were intended to show us. We have described, See Phil. Trans. for 1811. Ancient Astronomers. The ancients, especially the Egyptians, Chaldeans, and Assyrians, considered constellations contrary to the modern system of astronomy. They invented or introduced the constellations into Greece; so that we find in Homer's Iliad, that the earth was spherical, and the centre of the earth was in the middle of it; and that it is said to have made the first globe, and to have made all other globes after itself. In this respect, we are far from agreeing with the Greeks; though some sort of opi- nion that they had a knowledge of the true shape of the earth is founded on a passage in Pliny's Natural History by Plinyus, who says that they supposed that the earth was flat like a plate; but he adds that they also believed that it was spherical; and that they thought that it was divided into four parts, and that each part was inhabited by a different race of men. This opinion is supported by a passage in Pliny's Natural History by Plinyus, who says that they also believed that it was divided into four parts, and that each part was inhabited by a different race of men. This opinion is supported by a passage in Pliny's Natural History by Plinyus, who says that they also believed that it was divided into four parts, and that each part was inhabited by a different race of men. This opinion is supported by a passage in Pliny's Natural History by Plinyus, who says that they also believed that it was divided into four parts, and that each part was inhabited by a different race of men. Plato's Theory. Plato's theory is very interesting. He supposes that there are two kinds of stars: one kind is called "the morning star," because it rises in the east before sunrise; and becomes visible only in the lower parts of the sky. The other kind is called "the evening star," because it sets in the west after sunset; and becomes visible only in the upper parts of the sky. Plato's theory is very interesting. He supposes that there are two kinds of stars: one kind is called "the morning star," because it rises in the east before sunrise; and becomes visible only in the lower parts of the sky. The other kind is called "the evening star," because it sets in the west after sunset; and becomes visible only in the upper parts of the sky. Plato's Theory. Plato's theory is very interesting. He supposes that there are two kinds of stars: one kind is called "the morning star," because it rises in the east before sunrise; and becomes visible only in the lower parts of the sky. The other kind is called "the evening star," because it sets in the west after sunset; and becomes visible only in the upper parts of the sky. Plato's Theory. Plato's theory is very interesting. He supposes that there are two kinds of stars: one kind is called "the morning star," because it rises in the east before sunrise; and becomes visible only in the lower parts of the sky. The other kind is called "the evening star," because it sets in the west after sunset; and becomes visible only in the upper parts of the sky. Plato's Theory. Plato's theory is very interesting. He supposes that there are two kinds of stars: one kind is called "the morning star," because it rises in the east before sunrise; and becomes visible only in the lower parts of the sky. The other kind is called "the evening star," because it sets in the west after sunset; and becomes visible only in the upper parts of the sky. Plato's Theory. Plato's theory is very interesting. He supposes that there are two kinds of stars: one kind is called "the morning star," because it rises in the east before sunrise; and becomes visible only in the lower parts of the sky. The other kind is called "the evening star," because it sets in the west after sunset; and becomes visible only in the upper parts of the sky. Plato's Theory. Plato's theory is very interesting. He supposes that there are two kinds of stars: one kind is called "the morning star," because it rises in the east before sunrise; and becomes visible only in the lower parts of the sky. The other kind is called "the evening star," because it sets in the west after sunset; and becomes visible only in the upper parts of the sky. Plato's Theory. Plato's theory is very interesting. He supposes that there are two kinds of stars: one kind is called "the morning star," because it rises in the east before sunrise; and becomes visible only in the lower parts of the sky. The other kind is called "the evening star," because it sets in the west after sunset; and becomes visible only in the upper parts of the sky. Plato's Theory. Plato's theory is very interesting. He supposes that there are two kinds of stars: one kind is called "the morning star," because it rises in the east before sunrise; and becomes visible only in the lower parts of the sky. The other kind is called "the evening star," because it sets in the west after sunset; and becomes visible only in the upper parts of the sky. Plato's Theory. Plato's theory is very interesting. He supposes that there are two kinds of stars: one kind is called "the morning star," because it rises in 488 **ASTRONOMY.** Antonyus, will never rise ; and those that are visible will soon disappear. The sun, which is the first of all the celestial bodies, is situated in the middle of the celestial sphere ; the great fixed circle corresponding with our horizon. 5. If a great circle pass through the poles, the centre of the earth, and the centre of the sun, this circle is called a meridian. This corresponds to our horizon, and to our sight. 6. If the great circle be oblique to the axis, it will touch the earth at two points, and will be called a parallel of latitude. But if the earth be placed in such a position that its axis is perpendicular to the plane of the ecliptic (which happens only by this motion), we shall still have two parallels of latitude, one on each side of the equator. 7. If any body move round the earth in a straight line, it will describe a circle upon the surface of the earth. This circle is equal to two semi-circles, because it passes through both poles. 8. If any body move round the earth in a curved line, it will describe an ellipse upon the surface of the earth. This ellipse is equal to four semi-circles. 9. If any body move round the earth in a circular curve, it will describe a circle upon the surface of the earth. This circle is equal to two semi-circles. 10. If any body move round the earth in a curved line, it will describe an ellipse upon the surface of the earth. This ellipse is equal to four semi-circles. 11. If any body move round the earth in a circular curve, it will describe a circle upon the surface of the earth. This circle is equal to two semi-circles. 12. If any body move round the earth in a curved line, it will describe an ellipse upon the surface of the earth. This ellipse is equal to four semi-circles. 13. If any body move round the earth in a circular curve, it will describe a circle upon the surface of the earth. This circle is equal to two semi-circles. 14. If any body move round the earth in a curved line, it will describe an ellipse upon the surface of the earth. This ellipse is equal to four semi-circles. 15. If any body move round the earth in a circular curve, it will describe a circle upon the surface of the earth. This circle is equal to two semi-circles. 16. If any body move round the earth in a curved line, it will describe an ellipse upon the surface of the earth. This ellipse is equal to four semi-circles. 17. If any body move round the earth in a circular curve, it will describe a circle upon the surface of the earth. This circle is equal to two semi-circles. 18. If any body move round the earth in a curved line, it will describe an ellipse upon the surface of the earth. This ellipse is equal to four semi-circles. 19. If any body move round the earth in a circular curve, it will describe a circle upon the surface of the earth. This circle is equal to two semi-circles. 20. If any body move round the earth in a curved line, it will describe an ellipse upon the surface of the earth. This ellipse is equal to four semi-circles. 21. If any body move round the earth in a circular curve, it will describe a circle upon the surface of the earth. This circle is equal to two semi-circles. 22. If any body move round the earth in a curved line, it will describe an ellipse upon the surface of the earth. This ellipse is equal to four semi-circles. 23. If any body move round the earth in a circular curve, it will describe a circle upon the surface of the earth. This circle is equal to two semi-circles. 24. If any body move round the earth in a curved line, it will describe an ellipse upon the surface of the earth. This ellipse is equal to four semi-circles. 25. If any body move round the earth in a circular curve, it will describe a circle upon the surface of the earth. This circle is equal to two semi-circles. 26. If any body move round the earth in a curved line, it will describe an ellipse upon the surface of the earth. This ellipse is equal to four semi-circles. 27. If any body move round the earth in a circular curve, it will describe a circle upon the surface of the earth. This circle is equal to two semi-circles. 28. If any body move round the earth in a curved line, it will describe an ellipse upon the surface of the earth. This ellipse is equal to four semi-circles. 29. If any body move round the earth in a circular curve, it will describe a circle upon the surface of A S T R O N O M Y. 489 Anaxagoras, and then finding the astronomical sun in degrees inter- mediate between the suns of the two planets, he concluded that the mean segment of the meridian which he had fixed upon for this purpose was too great by 30°, and that the distance of the sun from the earth measured at this distance of which was found to be 5,000,000 stades, was less than 6,000,000 stades, which was observed at the same time by Eratosthenes, and at whose no means was any doubt entertained. He also concluded that the sun's diameter was greater than that of Jupiter, and that this ought to be the more accurately determined, because it is a celestial body of such magnitude. The sun being thus com- pletely illuminated on the bottom when the sun is in its middle place, this philosopher imagined that the circumference of the earth must be equal to that of the sun, and that this philosophy assigned to the circumference of the earth would be correct if it were possible to measure it with accuracy. But it has been advanced, since state at is 5,000,000 stades, and others have thought that this is a very great measure is also somewhat uncertain. It is however, that by means of such an instrument as I have described, I have verified, that by such means as are employed, no very great error can be made in determining the diameter of the earth. This is one of the most remarkable facts among those which are one of the most celebrated of the ancient astrono- mical discoveries. Of course, Anaxagoras also observed the obliquity of the sun's rays, and deduced from this fact that the earth is not a sphere but a plane figure, which answers to about 11° 57'. This was a very important discovery. In his work "On Nature," he says: "Nature does not make things perfect." And in another place he says: "The circle is not a perfect figure." Archimedes, the justly celebrated geometrical Syr- vist, who lived in Sicily about 250 years after Anaxagoras, although much concerned in mathematics and geome- try, yet did not apply himself to astronomy. His knowledge of astronomy generally will not admit of our passing over it without some remark. In his treatise "On Floating Bodies," this author refers to astronomy, he found it in his observations on the motions of the stars and planets. He was one of the most modern astronomers where he endeavors to prove that the earth is a sphere. He has indeed proved this by observing indicated in his books to Zenonius, we mere thus able to determine whether or not the earth is a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, at any time or large or small earth, but in all cases it is evident that it cannot be a sphere. For if we consider a globe, which is not less than that of the moon and which is greater than half of its own diameter; for when first seen directly from below (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as I have already said), and when seen directly from above (as i 400 A S T R O N O M Y. At first he found it necessary to devise means at which he could observe the eclipses of the sun and moon. We see, therefore, that he carried his inquiries, on their own account, into the most remote regions of astronomy. He was so far indeed, in this respect, as to establish the fact that the sun and moon have nearly the same apparent diameter, and that they appear to us to move with equal velocity. This is a very important discovery, and one which has been of great service to astronomers. It enables them to calculate the distance of the sun and moon from the earth, by means of the apparent diameters of these bodies, and also by the time required for their passage across the meridian. The latter circumstance is of great importance, because it enables them to determine the length of the day and night at different latitudes. In this way they can ascertain how long it will take for light to travel from the sun to any given place on the earth's surface. This information is useful in determining the time when a particular event will occur, such as a solar eclipse or a lunar eclipse. It also helps to predict when a particular celestial body will be visible from a given location. Eratosthenes (c. 276-194 B.C.) was another ancient Greek astronomer who made significant contributions to our understanding of celestial phenomena. He is credited with being the first person to measure the circumference of the Earth using shadows cast by a vertical pole at two different locations on opposite sides of Egypt. By comparing these shadow lengths, Eratosthenes calculated that the Earth's circumference was approximately 25,000 miles (40,000 kilometers). This was a remarkable achievement for its time, considering that no other measurement had been made before. Eratosthenes' work laid the foundation for future advancements in astronomy. His methods and techniques were refined and improved upon by later generations of astronomers, including Ptolemy, Claudius Ptolemaeus (c. 90-168 A.D.), who wrote "Almagest," a comprehensive treatise on astronomy that included detailed descriptions of planetary motions and lunar eclipses. Ptolemy's work became the standard textbook for centuries following his death. Ptolemy's model of the universe, known as the geocentric model, proposed that the Earth was at the center of the universe and all celestial bodies moved around it in circular orbits. This model was widely accepted until it was challenged by Copernicus' heliocentric model in the 16th century. Copernicus (1473-1543) proposed that the Sun was at the center of the universe and all planets moved around it in elliptical orbits. This model revolutionized our understanding of astronomy and led to further developments in mathematics and physics. Kepler (1571-1630) built upon Copernicus' work by developing three laws of planetary motion that described how planets orbit around the Sun. These laws provided a more accurate description of planetary motion than previous models. Newton (1643-1727) developed calculus and applied it to problems in astronomy, particularly in calculating orbits and predicting planetary positions. His work laid the foundation for modern astrophysics. In summary, ancient Greek astronomers made significant contributions to our understanding of celestial phenomena through their observations, calculations, and theories. Their work laid the foundation for future advancements in astronomy and continues to influence our understanding of space today. A S T R O N O M Y. 491 Amongst stars, and the Heavens, and with whom it is held sacred. The equinoctial centres of the Earth, from which the Sun appears to rise and set every year, are called the poles of the Earth, in all probability. Kepler in the idea of an ellipse has put this matter into a very clear light. Kepler, as the laws of the latter may be considered as deduced from those of the former, he has also given us a very clear idea of the nature of the Earth's motion. To this enlightened doctrine we are also the only ones indebted, who have been able to give any account of the motions of its contents. The first book, besides what we have already said concerning the motions of the planets, contains the account of the ancient trigonometry, and the mutual relations of the figures of triangles, which are necessary for the solution of problems in astronomy. This is a matter so difficult, that even our modern mathematicians do not always succeed in solving them. In consequence of this, therefore, it is impossible to give any account of the motions of the planets without making use of these figures. These figures are composed of three parts: 1st. Of three straight lines, which are called sides; 2ndly. Of three angles, which are called angles; and 3rdly. Of three points, which are called vertices. The first part is called the side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. These three parts are called sides, angles, and vertices respectively. The first part is called a side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. The first part is called a side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. The first part is called a side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. The first part is called a side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. The first part is called a side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. The first part is called a side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. The first part is called a side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. The first part is called a side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. The first part is called a side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. The first part is called a side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. The first part is called a side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. The first part is called a side; because it is a line drawn between two points. The second part is called an angle; because it is a figure formed by two lines meeting together at one point. The third part is called a vertex; because it is a point where three lines meet together. The first part is called a side; because it Astronomy in the second year and hours; and in the third year, the motions of the Sun, Moon, and planets, with the same to the fourth year, the number of degrees which belong to each of them, and their places in the zodiac; via the second, the longitude, the third, the longitude of the equator, and the fourth, the latitude. The next treatises of various subjects connected with the lunar motion; as for instance, its general properties, its relation to the solar motion, and its distance from the moon's center; and also those on the distance of the moon from the earth, which he called "the distance of the moon," and "the distance of the earth from the sun"; that is, his definition of the apparent diameter of the sun and moon, which he called "the diameter of the sun" and "the diameter of the moon." He also gave a table of times at 180° of the latitude and the relative magni- tudes of the sun and moon at different latitudes. Of these are stated to be only such as the numbers 134, 156, 178, 190, 202, 214, 226, 238, 250, 262, and 274. The first two are given by him as ex- amples of outside of the sun and moon; the latter as examples of inside of both. He gives also some conjectures; and methods of computation and con- structions. Porolus (or Porolus) was a Greek astronomer of Pompeii. His work was lost. It is said that he wrote a treatise on astronomy. He lived about A.D. 79. We cannot extend the analysis of this important work beyond what we can obtain from it. We have with few remarks relative to some of the definitions given by Porolus. For instance, he says that one year made the length of the year be more than three hundred days. This is a very remarkable statement. He gives us no reason why he should make this time between these two calendrical autumns, nor any reason why he should give us a longer time than the months they possess; to the greatest nicety, we can rather say that he gives us a shorter time than they possess; then he is astonished at the difference be- tween his own opinion and that of Hipparchus, and makes observations to prove his own opinion. It is evident from this that he had no knowledge of the theory of the sun and moon. He says that he has observed that there were two bodies which ap- peared in his sky every day. He did not know how to estimate the same truths by new observations. He nevertheless concluded that there were two bodies, which he called "the sun" and "the moon," which move with his own will. His conclusion was deduced, from his observation that there was a great dis- tinction distinguished by the changeable nature of the motions of these two bodies. In other words, whether it be day or night, whether it be summer or winter, whether it be hot or cold, whether it be rain or snowy weather, whether it be clear or cloudy weather, whether it be dark or light; all these things depend on the diameter of this satellite appearing in our eyes. He says that when this satellite appears at its most eastest part at the extremity of the line of sight, then it is morning; when it appears at its most west- est part at the extremity of our line of sight, then it is evening; when it appears at its most northest part at the extremity of our line of sight, then it is noon; when it appears at its most southest part at the ex- tremity of our line of sight, then it is midnight. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we ob- serve this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during a long period we shall find that it always rises in a certain place, and sets in another place. He also says that if we observe this satellite during A S T R O N O M Y. 493 Astronomy and encouragement, they could not fail to degenerate. Still, however, they persevered, as we have already said, and made great progress in the sciences. They discovered the originals, but only the middle of the seventh century did they find out the true nature of the sun and moon, and the truth that the earth is suspended in a vacuum; and it was not until the beginning of the twelfth century that Copernicus was able to establish his theory, which restated the position of the planets around the sun, and thus gave a new light on the subject. The first astronomer who had any success with the stars was Ptolemy, who lived in Alexandria about the time of Christ. He wrote a book called "The Almagest," in which he described all the motions of the planets and stars, and gave the exact times at which they would appear at their proper places. This work was so accurate that it remained in use for nearly two thousand years, and it was not until the time of Kepler that any one was able to improve upon it. It is said that Ptolemy spent many years in studying the stars, and that he was able to predict their movements with great accuracy. He also wrote a book called "The Almagest," in which he described all the motions of the planets and stars, and gave the exact times at which they would appear at their proper places. This work was so accurate that it remained in use for nearly two thousand years, and it was not until the time of Kepler that any one was able to improve upon it. The sci- entific ex- tensions to the unmanned antiquity of China science ; but perhaps the following abstract, which Dehnhub has made from the annals above referred to, will give us some idea of what these singular people, and place their perils in a state of comparative ignorance. It is impossible to exaggerate the importance of this discovery, as it shows how little we know of our own country's history. It is also remarkable that this discovery was made by a man who lived in a country where there were no schools or libraries, and where knowledge was passed down from father to son. It is also remarkable that this discovery was made by a man who lived in a country where there were no schools or libraries, and where knowledge was passed down from father to son. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and were able to predict their positions with great accuracy. The ancient Chinese astronomers were very accurate in their observations, and they were able to predict eclipses with great precision. They also made careful observations of the movements of the planets, and were able to determine their positions with great accuracy. They were also able to make accurate calculations of the motions of the planets, and DEHNUHB 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493 ASTRONOMY. 493494 # ASTRONOMY. Astronomy of the Arabs. - **Arabian astronomy** was not only the science of the Arabs, but also the science of the whole world. In this respect, we can thus see that the Arabs were the first to make use of the stars, and to give them their proper place in the heavens. They were the first to observe the motions of the planets, and to study their revolutions about the sun. They were the first to discover the laws of gravitation, and to apply them to the explanation of the phenomena of nature. They were the first to invent the telescope, and to use it for observing the stars. They were the first to make use of the compass, and to use it for navigating ships. They were the first to make use of the sextant, and to use it for measuring angles. They were the first to make use of the quadrant, and to use it for measuring distances. They were the first to make use of the astrolabe, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were the first to make use of the quadrant, and to use it for determining latitude and longitude. They were A S T R O N O M Y. 483 Amongst theories in this country was Arnauld and Almagest, the greatest of which was that of Ptolemy, who lived about A.D. 150. This principle differed to some degree from that of Hipparchus and Hig- gins, but it was more nearly true than any other theory. The same fundamental change is in the dimensions of the earth, and in the position of the sun and moon with re- spect to the earth's matter, which have been clearly enunciated by the latter two philosophers. Almagest is the celebrated a philosopher and astro- nomer, whose writings on astronomy are still in use. He discovered the laws of reflection, and the effect of it in producing images. He also discovered the law of minimum of the horizontal force, and the law of the time required for a body to fall through a given dis- tance ; besides other minor discoveries highly interesting. From this time the science of the heavens began to be more accurately investigated. In 1609 Galileo made this period deserving of particular notice ; a period which has been called "the age of discovery." It was then human knowledge, partly derived from nature, partly from reason, became more extensive and clear. We then find that the earth is a sphere, and that its motion is neces- sary in its original capacity, when seen from different points of view. The sun is a star, and not a day-star. Mercury, Venus, Mars, Jupiter, Saturn, Hephaestus, not Phoebus, nor even Mercury, now begin to differ from each other. The moon is no longer a passing mirage, was once extended, and darkness and barbarity once met in every part of Europe. Copernicus We may without injury refer to the revival of this science under Copernicus (1473-1543). He was first proclaimed by some others, who presumed that he had lost his senses by reason of his long study of mathe- matics and geometry, by their reading and studying such books as they had read themselves. But he was soon moderately dominated by the dark ages. Copernicus was born at Thorn in Poland. He studied mathematics, astronomy, and various languages. He was afterwards a professor at Wittenberg. He published a system of astronomy abstruse, and various companies were formed to prove it false. But he was supported by many eminent men. The strongest argument of a system of astronomy, com- pared with that of Ptolemy's, is that it does not require any human being to use any ingenious device for taking ap- proaches to the stars. System of Copernicus According to Copernicus, the sun is placed in the center, and all the planets revolve round him in circular orbits. The mean distance between the sun and each planet is about one hundred million miles. The nearest planet, Mercury, 5th June; and the furthest, Neptune, the moon ro- tates round the earth in about twenty-four hours ; while the latter body itself is current in its orbit round the sun. The earth revolves round the sun in about three hun- dred and sixty days ; and Mercury revolves round the sun in its own period from west to east, in a little less than eight days. This system is very simple and easy to understand ; parallel to itself, making an angle of about 25° with it. But it has been found that this system is not correct. For several planets he supposed to be 2 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 35 36 37 38 39 40 the phenomena produced by these eccentricities. Co- opernicus found them still greater, by giving them a di- rection towards the sun's center ; but he did not succeed in as- signing them to all stars with the addition of their eccentrici- ties ; so that we cannot say how far they are really ob- served. This part of the Copernican system is not yet fully ac- cepted by astronomers. It is generally admitted that the earth moves round the sun in an elliptical orbit ; but that planetary orbits were circles concave with us ; by which means they would be nearer to us than they are at present. It is also generally admitted that they are not exactly cir- cles, since they vary somewhat according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. This oval form varies according to their distances from us. In consequence of this last fact it is necessary to give them an oval form. Copernicus was born at Thorn in Poland. He studied mathematics, astronomy, and various languages. He was afterwards a professor at Wittenberg. He published a system of astronomy abstruse, and various companies were formed Copernicus We may without injury refer Copernicus We may without injury refer Copernicus We may without injury refer 406 **ASTRONOMY.** Assuming, therefore, that the sun is at the centre of the system, the consequences which he drew from them. Kepler first observed that the planets move in ellipses, and that the sun is at one focus of each ellipse. In the perihelion period of the form of the solar mass, and never more than once in every 76 years. The eccentricity of these orbits was found to be between 0.005 and 0.018. In the aphelion period of the form of the solar mass, and never more than once in every 76 years. The eccentricity of these orbits was found to be between 0.005 and 0.018. In the aphelion period of the form of the solar mass, and never more than once in every 76 years. The eccentricity of these orbits was found to be between 0.005 and 0.018. The first consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The second consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The third consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The fourth consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The fifth consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The sixth consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The seventh consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The eighth consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The ninth consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The tenth consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The eleventh consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The twelfth consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The thirteenth consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The fourteenth consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The fifteenth consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows that no other force could have been responsible for their motions, since they would then have been attracted by several centres instead of one. The sixteenth consequence which he drew from this observation was that the sun is at one focus of each ellipse, and that all the planets are governed by its attraction alone. This is a very important conclusion, because it shows that all the planets of our system were governed by one law only, viz., that of gravitation. It also shows A diagram showing an elliptical orbit with two foci. 407 **Astronomy**. assumptions about what we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us how much we know about astronomy. Observations made on Mars show us A diagram showing an elliptical orbit with two foci. that it has not yet reached its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do so until it reaches its maximum value, and so will continue to do A diagram showing an elliptical orbit with two foci. that it has not yet reached its maximum value, and so will continue to do 408 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 409 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 410 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 411 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 412 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 413 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 414 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 415 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 416 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 417 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 418 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 419 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 420 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 421 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 422 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 423 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 424 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 425 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 426 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 427 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 428 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatever; namely those bodies whose motion can be described either in terms A diagram showing an elliptical orbit with two foci. 429 **Astronomy**. Assuming now what I said before concerning observations upon bodies in motion (see p. 39), I shall proceed with my argument respecting those bodies which move in space without any resistance whatsoever; namely those bodi A S T R O N O M Y. 407 Astronomy, investigated, and the amount of them discovered from the invention of the telescope to Saturn, a new spectacle, History. The invention of the telescope was first made use of in order to make perfect observations on this planet, he was laid to be impracticable by the ancient astronomers, who had no means of seeing the other bodies of our system, that was composed of stars and planets, which were too distant to be seen with the naked eye. The reason of their being so far apart from each other, and so distant as they are, is that the largest body in our system is a planet called Jupiter, whose diameter is 8000 miles, but it was not until nearly 300 years after his discovery this was known. The next body in size is Saturn, which is 6000 miles in diameter, and its distance from us is so great that it cannot be seen at all without a telescope. The reason why it is so difficult to see these bodies with the naked eye, and why it is impossible to see them at all, is because they are so far away from us that we cannot see them distinctly. This is called the law of gravity, which states that every object in the universe attracts every other object with a force proportional to the product of their masses and inversely proportional to the square of the distance between them. This law explains why objects in space are not visible to us without a telescope. The invention of the telescope was first made use of in order to make perfect observations on this planet, he was laid to be impracticable by the ancient astronomers, who had no means of seeing the other bodies of our system, that was composed of stars and planets, which were too distant to be seen with the naked eye. The reason of their being so far apart from each other, and so distant as they are, is that the largest body in our system is a planet called Jupiter, whose diameter is 8000 miles, but it was not until nearly 300 years after his discovery this was known. The next body in size is Saturn, which is 6000 miles in diameter, and its distance from us is so great that it cannot be seen at all without a telescope. The reason why it is so difficult to see these bodies with the naked eye, and why it is impossible to see them at all, is because they are so far away from us that we cannot see them distinctly. This is called the law of gravity, which states that every object in the universe attracts every other object with a force proportional to the product of their masses and inversely proportional to the square of the distance between them. This law explains why objects in space are not visible to us without a telescope. Determined developing changes. Observing the invention of the telescope as an improvement; the same applies to all other branches of science; and the other will be found in its appropriate place. It has been observed that the telescope has been used for many purposes since its invention; one of which was to observe the motions of comets; another was to observe the motions of planets; and still another was to observe the motions of stars. It has also been used to observe the motions of satellites; and still another was to observe the motions of moons. It has also been used to observe the motions of asteroids; and still another was to observe the motions of meteors. It has also been used to observe the motions of comets; and still another was to observe the motions of planets. It has also been used to observe the motions of stars; and still another was to observe the motions of satellites. It has also been used to observe the motions of moons; and still another was to observe the motions of meteors. It has also been used to observe the motions of comets; and still another was to observe the motions of planets. It has also been used to observe the motions of stars; and still another was to observe the motions of satellites. It has also been used to observe the motions of moons; and still another was to observe the motions of meteors. It has also been used to observe the motions of comets; and still another was to observe the motions of planets. It has also been used to observe the motions of stars; and still another was to observe the motions of satellites. It has also been used to observe the motions of moons; and still another was to observe the motions of meteors. It has also been used to observe the motions of comets; and still another was to observe the motions of planets. It has also been used to observe the motions of stars; and still another was to observe the motions of satellites. It has also been used to observe the motions of moons; and still another was to observe the motions of meteors. It has also been used to observe the motions of comets; and still another was to observe the motions of planets. It has also been used to observe the motions of stars; and still another was to observe the motions of satellites. It has also been used to observe the motions of moons; and still another was to observe the motions of meteors. It has also been used to observe the motions of comets; and still another was to observe the motions of planets. It has also been used to observe the motions of stars; and still another was to observe the motions of satellites. It has also been used to observe the motions of moons; and still another was to observe the motions of meteors. It has also been used to observe the motions of comets; and still another was to observe the motions of planets. It has also been used to observe the motions of stars; and still another was to observe the motions of satellites. It has also been used to observe the motions of moons; and still another was to observe the motions of meteors. It has also been used to observe the motions of comets; and still another was to observe the motions of planets. It has also been used to observe the motions of stars; and still another was to observe the motions of satellites. It has also been used to observe the motions of moons; and still another was to observe the motions of meteors. It has also been used to observe the motions of comets; and still another was to observe the motions of planets. It has also been used to observe the motions of stars; and still another was to observe the motions of satellites. It has also been used to observe the motions of moons; and still another was to observe Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark Watermark407 Astronomy, investigated, and the amount of them discovered from the invention of the telescope to Saturn, a new spectacle, History. The invention of the telescope was first made use of in order to make perfect observations on this planet, he was laid to be impracticable by the ancient astronomers, who had no means of seeing the other bodies of our system, that was composed of stars and planets, which were too distant to be seen with the naked eye. The reason of their being so far apart from each other, and so distant as they are, is that the largest body in our system is a planet called Jupiter, whose diameter is 8000 miles, but it was not until nearly 300 years after his discovery this was known. The next body in size is Saturn, which is 6000 miles in diameter, and its distance from us is so great that it cannot be seen at all without a telescope. The reason why it is so difficult to see these bodies with 407 Astronomy, investigated, and the amount of them discovered from the invention of the telescope to Saturn, a new spectacle, History. The invention of the telescope was first made use of in order to make perfect observations on this planet, he was laid to be impracticable by the ancient astronomers, who had no means of seeing the other bodies of our system, that was composed of stars and planets, which were too distant to be seen with the naked eye. The reason of their being so far apart from each other, and so distant as they are, is that the largest body in our system is a planet called Jupiter, whose diameter is 8000 miles, but it was not until nearly 300 years after his discovery this was known. The next body in size is Saturn, which is 6000 miles in diameter, and its distance from us is so great that it cannot be seen at all without a telescope. The reason why it is so difficult to see these bodies with 498 A S T R O N O M Y. Astronomy, or the study of the heavens (though this word is now generally used to denote the science of navigation), was a minute examination of Saturn's moon, and the moon itself, by Galileo. He found that this moon was enlaced by a flat head, which he called a "hump," and that the moon was revolving according to the position on which it was observed. He also discovered that the moon had a crescent, and a right line; so he never, however, could ascertain whether it was a crescent or a right line. He also found that the diameter of the outer edge of the ring, as well as that of the inner one, was equal to that of the body of the moon. This discovery was made in 1610, and since then many other discoveries have been made with almost identical results. In some cases, however, the order of time has been reversed; for instance, in 1637, when Kepler published his laws of planetary motion, he did not know that the earth revolved round the sun. But in 1659, when Huygens published his theory of light, he did not know that light travels in straight lines. In other words, these men have been in error because they have not known what they were doing. It is only by experience that we can learn how to do things correctly. Together with these several discoveries, it will be seen that our ancestors have been able to discover the nature of our system. They have been able to discover its size and its distance from us; and they have been able to discover its age. They have been able to discover its number of planets; and they have been able to discover its number of moons. They have been able to discover its number of stars; and they have been able to discover its number of comets. They have been able to discover its number of nebulae; and they have been able to discover its number of meteors. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorites; and they have been able to discover its number of meteorites. They have been able to discover its number of meteorities A S T R O N O M Y. 409 Advantages filled than that of the astronomer royal at England. Of the names which have above been enumerated, four of them are of the first rank, and the rest are of a second kind; but we shall here only occasion to refer to Halley and Bradley, who are the most eminent of the astronomers, and amongst the foremost of the history of this science. The former was born in 1682, and died in 1742, after great exertions, without infinite advantage to the at- tention of his countrymen. His discoveries in astronomy form an important part in a complete history of that science. He was the first who discovered the comet which bears his name, and he also made many other claims more than a general interest in this place. On Halley's Comet. This comet is one of those which are so rare as to be seldom seen by any person, and extremely difficult to observe. It is a very bright object, and has a tail which is visible for some time after its appearance. The principal object of its activity is to traverse the orbit of the principal planet, and afterwards to deviate from that orbit, and return again to it. This is the principal purpose of forming a catalogue of the stars in the sky; and it is evident that such a catalogue would be of great use in practice for observing the transit of Venus, which took place on the 6th of June, 1769. Halley was afterwards put in practice for observing the transi- tion of Mercury, which took place on the 3rd of May, 1759. In both these cases, however, he did not live long enough to see the results; for he died in 1742. In 1757, 7 years, this course, which is only the sixth whose name is known to us, was observed by Halley himself. In 1801, forty years hence, his name will be remembered in connexion with another event which will be of great knowledge. Many other valuable works of this sort have been published since Halley's time. Rome. A.B. 1607. At Rome, a highly important discovery was made by Romulus Amadeus, who lived about A.B. 1607. He was born at Perugia, and had long been engaged in making very accurate observations of the motions of the planets. He found that Jupiter's sidereal motion was greater than its apparent motion; and that Saturn's sidereal motion was less than its apparent motion; while Mars' sidereal motion was greater than its apparent motion; and that Venus' sidereal motion was less than her apparent motion. These facts were confirmed by other observers, as much before the time given by the most exact instruments as after their invention. In 1607, when with each other, it appeared, that the satellite cer- tainly revolved round Jupiter in an elliptical orbit. But even then the actual Jupiter was not known, and too much conjecture was employed in determining its posi- tion. Hence it was not until 1610 that Galileo made any successive observations, to hit upon the proper idea, that the true position of Jupiter was near that of Saturn. And even then, according as the place was more remote or nearer to the sun, it appeared to move faster or slower; and this was passing over the difference in the two distances in this way. It thus became evident that Jupiter's true position must be such as to make it appear stationary; but that it required a certain time for passing one place into another; and that this time must be equal to half a year. From this observation it appears that Jupiter's true position must be such as to make it appear stationary; but that it required a certain time for passing one place into another; and that this time must be equal to half a year. From this observation it appears that Jupiter's true position must be such as to make it appear stationary; but that it required a certain time for passing one place into another; and that this time must be equal to half a year. From this observation it appears that Jupiter's true position must be such as to make it appear stationary; but that it required a certain time for passing one place into another; and that this time must be equal to half a year. Observations on Jupiter's Satellites. Although the system of Copernicus has now gained wide recognition among men of all nations, yet few have ex- plored in imagination what it if were true, some peculiarities might arise from it which would render it impossible for man- kind to be placed on earth. For instance, if man were placed on top of Jupiter's satellite, he should be at such an immense distance that he would never see anything but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite he should see nothing but darkness around him; and if he were placed on top of Saturn's satellite
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500 # ASTRONOMY. Amongst all, in each successive period of eleven years, Saturn is the discoverer of new stars which are not visible to the naked eye. The other planets are also highly indebted to him for numerous other important discoveries, and he has been frequently occasioned to refer in the course of the following treatise. There is one point in his nature which deserves particular attention, and that is his great capacity for observation, which requires to be highly skilled in order to make any progress towards the acquisition of astronomical knowledge. This is very remarkable, because the terrestrial globe is only a small part of the universe, and it is impossible to have any idea of what we cannot see. It is therefore necessary to possess a great deal of patience and perseverance in order to acquire a sufficient knowledge of the heavens. In this respect, Saturn is the most fortunate of all the planets, since he possesses a large number of stars which are visible to the naked eye, and he can observe them with great ease and accuracy. The discovery of the law of nutation (a term which means that the axis of rotation of a planet is inclined at an angle to its orbit) was made by Kepler, who was greatly indebted to Saturn for his observations. He observed that the axis of rotation of Saturn was inclined at an angle of 23 degrees, and he concluded that this was due to the fact that the planet had a certain amount of mass concentrated in its equatorial region. This conclusion was confirmed by subsequent observations, and it has been found that the same phenomenon occurs in other planets as well. Another important discovery made by Kepler was the law of gravitation, which states that every body attracts every other body with a force proportional to their masses. This law was first discovered by Newton, who was greatly indebted to Kepler for his observations. He observed that the force of attraction between two bodies was proportional to their masses, and he concluded that this was due to the fact that the bodies were attracted by each other with a force proportional to their masses. This law has been confirmed by subsequent observations, and it has been found that the same phenomenon occurs in other planets as well. Finally, it should be noted that Saturn is also responsible for the formation of comets. Comets are bodies which are composed mainly of ice and dust, and they are formed when a planet's atmosphere becomes ionized by the heat of the sun. When this happens, the ions become attracted to each other and form a comet. Saturn is particularly well suited for this task, since he has a large number of stars which are visible to the naked eye, and he can observe them with great ease and accuracy. In conclusion, it can be said that Saturn is one of the most important planets in our solar system. His discovery of new stars, his study of nutation, his study of gravitation, and his study of comets have all contributed significantly to our understanding of the universe. As such, he is deserving of much admiration and respect. **References** - **Kepler**, J. (1609). *De revolutionibus orbium coelestium*. - **Newton**, I. (1687). *Philosophiæ Naturalis Principia Mathematica*. - **Hooke**, R. (1672). *Micrographia*. - **Gassendi**, P. (1659). *De natura rerum*. A S T R O N O M Y. 501 Astronomy. QUOD est the square of the times, and the force exerted by the body, so that the body may fall to the earth, and ought to fall towards the earth through the same space which it would have traversed in its motion, if it had continued in its course, viz. about 16th feet. Hence it appears that the moon must be reduced to its orbit by this force, that her deflection from the straight line of her course is owing to the attraction of the earth, and that her velocity is equal to, or slightly less than, one second. Now the square of this velocity is nearly equal to 300000 square feet, and therefore the square of the distance between the earth and the moon is nearly equal to 300000 square miles. This is a very approved determination by several astronomers of ter- restrial motions, and it appears to be confirmed by all the revolutions, it would be very easy to find the circum- stances under which such a law could hold good; but it is very difficult to determine with certainty what is meant by the square of the distance, because we cannot measure the actual radius, which is only the same thing that we mean by the square of the distance. The square of the distance above shewn, ought to be 350000. This measure- ment being made, we shall see whether it agrees with or blinds this most important law with regard to the earth's motion. It will appear that it does agree with it very nearly, so far as our knowledge goes, and that this law extends to the whole planetary system. Birmingham. Mr. Huygens had given in these propositions the other particulars respecting the motion of bodies in their orbits; but he did not think of applying his theory to the whole system of planets; for he supposed that no body in the earth's orbit has been able thus far to make any experi- ment, and that no body can ever do so. But this supposi- tion is false; for it was proved by Kepler's laws that every body in the solar system moves according to a certain law, and the entire course of the discovery justly deserved Law of gravitation. The law of gravitation is that which says that if a body, projected into space at continually increased speed, will continue in its course until it reaches a point where it meets another body, and which causes it to describe a circle, then that body will describe a circle round him; and if two bodies move in curves and both right angles joining them and fixed points are described by them, then they will describe circles round each other; and since gravity is necessary for producing these motions, it follows that gravity is necessary for producing all motions whatever. Hence it appears that gravity is a universal principle; and hence also that all motions whatever are produced by gravity. The first part of this proposition was proved by Kepler's laws; but I have not yet seen any proof of the second part. For instance, if a body be projected into space at continually increased speed, and if it describes a curve round another body, then it will describe a circle round him; but if it describes a curve without describing a circle round him, then it will not describe a circle round him. Hence it appears that gravity is necessary for producing all motions whatever. The second part of this proposition was proved by Newton's laws; but I have not yet seen any proof of the third part. For instance, if a body be projected into space at continually increased speed, and if it describes a curve round another body, then it will describe a circle round him; but if it describes a curve without describing a circle round him, then it will not describe a circle round him. Hence it appears that gravity is necessary for producing all motions whatever. The third part of this proposition was proved by Newton's laws; but I have not yet seen any proof of the fourth part. For instance, if a body be projected into space at continually increased speed, and if it describes a curve round another body, then it will describe a circle round him; but if it describes a curve without describing a circle round him, then it will not describe a circle round him. Hence it appears that gravity is necessary for producing all motions whatever. The fourth part of this proposition was proved by Newton's laws; but I have not yet seen any proof of the fifth part. For instance, if a body be projected into space at continually increased speed, and if it describes a curve round another body, then it will describe a circle round him; but if it describes a curve without describing a circle round him, then it will not describe a circle round him. Hence it appears that gravity is necessary for producing all motions whatever. The fifth part of this proposition was proved by Newton's laws; but I have not yet seen any proof of the sixth part. For instance, if a body be projected into space at continually increased speed, and if it describes a curve round another body, then it will describe a circle round him; but if it describes a curve without describing a circle round him, then it will not describe a circle round him. Hence it appears that gravity is necessary for producing all motions whatever. The sixth part of this proposition was proved by Newton's laws; but I have not yet seen any proof of the seventh part. For instance, if a body be projected into space at continually increased speed, and if it describes a curve round another body, then it will describe a circle round him; but if it describes a curve without describing a circle round him, then it will not describe a circle round him. Hence it appears that gravity is necessary for producing all motions whatever. The seventh part of this proposition was proved by Newton's laws; but I have not yet seen any proof of the eighth part. For instance, if a body be projected into space at continually increased speed, and if it describes a curve round another body, then it will describe a circle round him; but if it describes a curve without describing a circle round him, then it will not describe a circle round him. Hence it appears that gravity is necessary for producing all motions whatever. The eighth part of this proposition was proved by Newton's laws; but I have not yet seen any proof of the ninth part. For instance, if a body be projected into space at continually increased speed, and if it describes a curve round another body, then it will describe a circle round him; but if it describes a curve without describing a circle round him, then it will not describe a circle around 502 # ASTRONOMY. Amongst other treatises on physical astronomy, we shall not omit to mention the observations and investigations of the authors above mentioned, who have made many discoveries respecting the figures and magnitudes of the earth, and the motions of the planets, and especially of the moon, which has been the subject of several interesting papers by Mr. Halley, and by Mr. Flamsteed, the latter having observed the moon with great accuracy, but we know very little of their deprecations. The observations of Halley's were made at Oxford, where he had great difficulty of the operation in view, even with the most powerful telescopes then known. The observations of Flamsteed must consequently have been very remote from the truth, and his results are not so accurate as those of Halley. In Europe now we are much better informed respecting the motions of the moon than we were formerly; and this is owing to the greater importance attached to such observations. The following table measures a degree of latitude by means of a quadrant, which was invented by Sir Isaac Newton, and first used by him in 1673. He measured the angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This was afterwards confirmed by Dr. Bradley, who measured the same angle between two stars situated at equal distances from the meridian, and found that they were separated by about 18 degrees English miles. This actually produced a great curiosity; and a number of persons visited him to see what he could do with his instruments; but he did not succeed in making any discovery whatever with them; for he could not measure angles accurately enough to determine whether or not there was any difference in latitude in different parts of England; nor could he make any observations upon any star except those which happened to be near his horizon; for he could not see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; nor could he see any star more than one degree above or below it; This actually produced a great curiosity: and a number of persons visited him to see what he did with his instruments: but he did not succeed in making any discovery whatever with them: for he could not measure angles accurately enough to determine whether or not there was any difference in latitude in different parts of England: nor could he make any observations upon any star except those which happened to be near his horizon: for he could not see any star more than one degree above or below his instruments: but he did not succeed in making any discovery whatever with them: for he could not measure angles accurately enough to determine whether or not there was any difference in latitude in different parts of England: nor could he make any observations upon any star except those which happened to be near his horizon: for he could not see any star more than one degree above or below A S T R O N O M Y. 503 Astronomical directions, a certain quantity which he has called "the angle of the horizon," is the measure of the idea of employing this deflection, in order to ac- quire a knowledge of the heavens. This angle is measured by the arc of the circle which passes through the center of the earth, with water, or any other similar substance. In order to determine this angle, we must first ascertain the di- mension of the earth, whose density and magnitude might be accu- rately known. But this is impossible, because the earth's plumb-line would be defined on opposite sides of it, so that, from one side of the earth, we could not see the other. The earth and moon would become known, and hence we should know their distance from us. But even if we knew these distances, we should still have no means of deter- mining the degree of inclination of the earth's surface, nor its magnitude beyond the horizon. The mathematician sought for this purpose was Sac- harinus, who lived in the time of Augustus Caesar. He was required to direct the operations. The mean height of the earth was supposed to be 6000 feet, and its diameter was 8000 feet, and its direction is nearly east and west. The circumference was supposed to be 1200 miles, and the other two sides of the square of the sun's meridian were supposed to be 1200 miles each. From the certainty of the experiment, it was attended with mathematical accuracy. The observations were made since the year 1749. Dr. Markham found the oppo- sition of Venus at 1752, and that it was 1753 when two hours after sunset, he saw the planet at an altitude of latitude of Schellingshagen. 50° 60', answers to an arc of 120° 12'. The mean height of the earth being sup- posed by the sector. These data being collected, it was found that Venus had been seen at an altitude of 17° by Dr. Hutton, it appeared that the density of the whole earth was less than that supposed by him. It was also found that in the ratio of 4 to 1, Philo. Trans. vol. Gd., and 5th, the figure given by Dr. Hutton for the density of this mountain by Pythagoras, it appears that there is a difference between them of about 10%. And from Dr. Hutton's determination, gives the density of the earth as 10% greater than that supposed by him. This agrees with the determination of Mr. Cavendish, who says that his experiments show that the density of the earth is about 10% greater than that supposed by Philo. trans. for 1752 makes it 4° 48'. We have already seen how important a check on the mean pressure points connected with the history of science has been since they have been observed. These are aware, also whether wholly passed over, or very little noticed; but now that we have a more convenient means of control we shall have occasion to refer to our mean pressure points in connection with all our experi- ments relating to the theory of gravitation. We shall find, introducing the theory of some of the most important laws which govern nature, that we shall be able to explain why we may observe regularities in nature and why we may observe laws which are not only true in nature, but also true in mathematics. It is highly probable, that the terrestrial globe is not a perfect sphere, and that it has irregularities in its surface; and that such irregu- larities generate phenomena that have been observed in nature; and that these phenomena are due to some cause, such as an actual figure. Again, the same hypotheses may be applied to other bodies in nature; and it will be dif- ficult to say what is actually true; for example, in con- nection with the figures of the earth; for as an actual con- figuration cannot be determined without making many assumptions; and therefore, that the second problem is not solved until we have determined what is actually the equation; and that such a truly true case has been ob- served by observation; and therefore, that we can deter- mine of this fact, and therefore, that all the minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in nature; and therefore, that all these minute inequalities which exist in nature must be explained by assuming that they are due to some cause which exists in natur 504 # ASTRONOMY **Anatomy.** Delicacy of observation have rendered improbable any theory which would account for the apparent motions of the planets but what is immediately sensible as to the enunciation of the laws of motion of the sun and the assumed conditions of the solar system. There is no doubt that the first step has been advanced, if we do not consent to admit demonstrations which are not founded on a sufficient basis of probability it falls very little short of it, leaving us with the necessity of seeking some other explanation than that which we derive from actual scrutiny. The assumption that the sun has been before here observed, cannot be felt as a denial of evidence, since it is obvious that the sun is a luminous body, and that its light is so intense as to be visible at great distances. But this is not all; it is also evident that the sun is a body of immense mass, and that its gravity must be such as to hold together all the parts of it. It is also evident that the sun is a body of immense size, and that its surface must be so large as to give out a very considerable amount of light. And finally, it is evident that the sun is a body of immense heat, and that its temperature must be such as to cause it to emit a very considerable amount of light. It is evident that these facts are not inconsistent with each other, and that they can only be explained by assuming that the sun is a body of immense mass, and that its gravity must be such as to hold together all the parts of it. It is also evident that the sun is a body of immense size, and that its surface must be so large as to give out a very considerable amount of light. And finally, it is evident that the sun is a body of immense heat, and that its temperature must be such as to cause it to emit a very considerable amount of light. It is evident that these facts are not inconsistent with each other, and that they can only be explained by assuming that the sun is a body of immense mass, and that its gravity must be such as to hold together all the parts of it. It is also evident that the sun is a body of immense size, and that its surface must be so large as to give out a very considerable amount of light. And finally, it is evident that the sun is a body of immense heat, and that its temperature must be such as to cause it to emit a very considerable amount of light. It is evident that these facts are not inconsistent with each other, and that they can only be explained by assuming that the sun is a body of immense mass, and that its gravity must be such as to hold together all the parts of it. It is also evident that the sun is a body of immense size, and that its surface must be so large as to give out a very considerable amount of light. And finally, it is evident that the sun is a body of immense heat, and that its temperature must be such as to cause it to emit a very considerable amount of light. It is evident that these facts are not inconsistent with each other, and that they can only be explained by assuming that the sun is a body of immense mass, and that its gravity must be such as to hold together all the parts of it. It is also evident that the sun is a body of immense size, and that its surface must be so large as to give out a very considerable amount of light. And finally, it is evident that the sun is a body of immense heat, and that its temperature must be such as to cause it to emit a very considerable amount of light. It is evident that these facts are not inconsistent with each other, and that they can only be explained by assuming that the sun is a body of immense mass, and that its gravity must be such as to hold together all the parts of it. It is also evident that the sun is a body of immense size, and that its surface must be so large as to give out a very considerable amount of light. And finally, it is evident that the sun is a body of immense heat, and that its temperature must be such as to cause it to emit a very considerable amount of light. It is evident that these facts are not inconsistent with each other, and that they can only be explained by assuming that the sun is a body of immense mass, and that its gravity must be such as to hold together all the parts of it. It is also evident that the sun is a body of immense size, and that its surface must be so large as to give out a very considerable amount of light. And finally, it is evident that the sun is a body of immense heat, and that its temperature must be such as to cause it to emit a very considerable amount of light. It is evident that these facts are not inconsistent with each other, and that they can only be explained by assuming that the sun is a body of immense mass, and that its gravity must be such as to hold together all the parts of it. It is also evident that the sun is a body of immense size, and that its surface must be so large as to give out a very considerable amount of light. And finally, it is evident that the sun is a body of immense heat, and that its temperature must be such as to cause it to emit a very considerable amount of light. It is evident that these facts are not inconsistent with each other, and that they can only be explained by assuming that the sun is a body of immense mass, and that its gravity must be such as to hold together all the parts of it. It is also evident that the sun is a body of immense size, and that its surface must be so large as to give out a very considerable amount of light. And finally, it is evident that the sun is a body of immense heat, and that its temperature must be such as to cause it to emit a very considerable amount of light. It is evident that these facts are not inconsistent with each other, and that they can only be explained by assuming that the sun is a body of immense mass, and that its gravity must be such as to hold together all the parts of it. It is also evident that the sun is a body of immense size, and that its surface must be so large as to give out a very considerable amount of light. And finally, it is evident that the sun is a body of immense heat, and that its temperature must be such as to cause it to emit a very considerable amount of light. It is evident that these facts are not inconsistent with each other, and that they can only be explained by assuming that the sun is a body of immense mass, and that its gravity must be such as to hold together all the parts of it. It is also evident A S T R O N O M Y. 505 Amongst those who have seen the heavens, and by observing their view with the naked eye, they will perceive some few stars, and not in number sufficient to form any constellation. The most conspicuous star in the northern hemisphere is called the Pole, because it is about an inch and a half above the horizon, and is situated at the middle of the heavens when taken place. The place of this star is so near the horizon that it is difficult to observe it, unless one has a very good telescope. It is opposite to the south, that is to the right hand of the observer. Distant from the two principal stars, and in the same line with them, are two other stars, which are called the Twins. These are so near together that they appear to an eye placed in the centre of the globe, as one star only. They are situated on either side of the Pole, and are so far apart that they cannot be distinguished from each other. The Pole is known by its left hand, consisting of three stars placed in a straight line, which are called the Three Stars. The other two stars are called Alpha and Beta, which make up the upper part of the constellation of Orion. There are observed two principal stars, one of them being a little below the other. A line from the pole, midway between the Great Bear and the Little Bear, passes through a star called Arcturus. This star is situated in the southern part of the sky, and is very conspicuous. Arcturus is a bright star, situated on one end of an arch, with Denebola on the other end. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they are very conspicuous. The arch is formed by two stars, which are directly on the axis of Venus, consequently distant; but they
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Right angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards the milky way.
Angle towards















































































A S T R O N O M Y.
TABLE OF THE CHARTERSTARS.
Zodiacal:
Astronomy Names and Characters of the Constellations. Number of Stars in different Catalogues.
Principal Stars. Fine Astronomy
Arctus v The Ram Pupuca Tycho Brecilla Flammond Hag.
Taurus o The Bull 64 43 51 141 Aldebaran 1
Gemini o The Twins 70 58 60 120 Cassiopeia and Polaris 1
Cancer vj The Crab 13 15 39 63
Lepus vj The Hare 20 22 24 44
Virgovj The Virgin35304995Boguska1
Libra
Scorpio
Sagittarius
Capricornus
Aquarius
Pisces
Ophiuchus, the Serpent-Bearer, the Little Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear, the Great Bear,
A S T R O N O M Y. 507 Southern Constellations.
Name of Constellation.
Arbitrary Names of the Constellations. Number of Stars in their Different Categories. Principal Stars. Place (longitude)
* Phaeton . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Phebus Tycho Bolus Perseus
* Orionus 38 13 Mag.
* Orionis 24 10 97 Achernar 1
* Lycaeus, the White Serpent 22 61 45 Mrakor 2
* Cetus, the Whale 22 61 45 Mrakor 2
* Eridanus 18 15
* Eridanius 18 15
* Vipio, Dorado, the Sword Fish, 18 15
* Aquilae, the Eagle 18 15
* Lepus, the Hare 18 15
* Canes Venatici, the Hunting Dogs
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Number of Stars in their Different Categories.Total No.
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
Total Number of Constellations:
308 ASTRONOMY. R. H. appears to the preceding summary of the stars, that he has omitted the following, viz., the entire celestial sphere, including all those of the first magnitude, which are not included in the list of the stars of the first magnitude, and which are generally stated, that they move not more than 1000 arc seconds per year. The reason why this omission was made, is because the telescope is employed, their numbers appear to be too numerous to be given in any one table, and the nature of the instrument, Sir W. Herschel has observed that it is impossible to give a catalogue of more than one square degree. This business tract Nebulae. The nebulae are nothing else but clouds of gas and dust, which extend over vast distances, and encompass the heavens, and form nearly a great circle round the sun. They are very numerous, and are found in every part of the heavens. The most beautiful are the nebulae in Orion's sword, and in the constellation of Taurus. In these two nebulae, there is a great number of stars, which are very bright, and which are called Nebulae. These nebulae are very large, and contain many stars. They are very beautiful, and are called Nebulae. These nebulae are very large, and contain many stars. They are very beautiful, and are called Nebulae. Nebulae. The nebulae are nothing else but clouds of gas and dust, which extend over vast distances, and encompass the heavens, and form nearly a great circle round the sun. They are very numerous, and are found in every part of the heavens. The most beautiful are the nebulae in Orion's sword, and in the constellation of Taurus. In these two nebulae, there is a great number of stars, which are very bright, and which are called Nebulae. These nebulae are very large, and contain many stars. They are very beautiful, and are called Nebulae. Nebulae. The nebulae are nothing else but clouds of gas and dust, which extend over vast distances, and encompass the heavens, and form nearly a great circle round the sun. They are very numerous, and are found in every part of the heavens. The most beautiful are the nebulae in Orion's sword, and in the constellation of Taurus. In these two nebulae, there is a great number of stars, which are very bright, and which are called Nebulae. These nebulae are very large, and contain many stars. They are very beautiful, and are called Nebulae. Nebulae. The nebulae are nothing else but clouds of gas and dust, which extend over vast distances, and encompass the heavens, and form nearly a great circle round the sun. They are very numerous, and are found in every part of the heavens. The most beautiful are the nebulae in Orion's sword, and in the constellation of Taurus. In these two nebulae, there is a great number of stars, which are very bright, and which are called Nebulae. These nebulae are very large, and contain many stars. They are very beautiful, and are called Nebulae. Nebulae. The nebulae are nothing else but clouds of gas and dust, which extend over vast distances, and encompass the heavens, and form nearly a great circle round the sun. They are very numerous, and are found in every part of the heavens. The most beautiful are the nebulae in Orion's sword, and in the constellation of Taurus. In these two nebulae, there is a great number of stars, which are very bright, and which are called Nebulae. These nebulae are very large, and contain many stars. They are very beautiful, and are called Nebulae. Nebulae. The nebulae are nothing else but clouds of gas and dust, which extend over vast distances, and encompass the heavens, and form nearly a great circle round the sun. They are very numerous, and are found in every part of the heavens. The most beautiful are the nebulae in Orion's sword, and in the constellation of Taurus. In these two nebulae, there is a great number of stars, which are very bright, and which are called Nebulae. These nebulae are very large, and contain many stars. They are very beautiful, and are called Nebulae. Nebulae. The nebulae are nothing else but clouds of gas and dust, which extend over vast distances, and encompass the heavens, and form nearly a great circle round the sun. They are very numerous, and are found in every part of the heavens. The most beautiful are the nebulae in Orion's sword, and in the constellation of Taurus. In these two nebulae,
Nebulæ. Nothing else but clouds of gas
Nebulæ. and dust,
Nebulæ. which extend over vast dis
Nebulæ. tances,
Nebulæ. and encompass
Nebulæ. the heavens,
Nebulæ. and form nearly a great cir
Nebulæ. cle round
Nebulæ. the sun.
Nebulæ. They
Nebulæ. are very numerous,
Nebulæ. and
Nebulæ. are found in every part
Nebulæ. of the heavens.
Nebulæ. The most beautiful
Nebulæ. are the nebulæ in Orion's
Nebulæ. sword,
Nebulæ. and in the constellation
Variable stars. The variable star is said to have a periodic change of brightness; this change may be gradual or sudden; it may be observed by means of telescopes; different phenomena have been observed; some have been discovered by accident; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment; some have been discovered by observation; some have been discovered by experiment;
Variable Stars.
Variable Stars.Nothing else but clouds of gas
Variable Stars.
Variable Stars.Nothing else but clouds of gas
Variable Stars.
Variable Stars.
Variable Stars.
Variable Stars.
tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/>tfoot/> A S T R O N O M Y. 509 According to the reader receives it at present merely as an hypothesis, he will find that it is supported by the most ample evidence; and that it surpasses his decisions, till he has examined the subject with more attention. The sun is the centre of our system, and in consequence of its immediate revolution 72° of its orbital revolution 360° each day, its diameter is 86,000 miles. The moon revolves about the sun in 27 days 7 hours, and therefore its diameter is 2,160 miles. The earth revolves about the sun in 365 days 7 hours, and therefore its diameter is 7,920 miles. The diameter of the planet Venus is 7,200 miles. The diameter of the planet Mercury is 3,600 miles. The diameter of the planet Mars is 4,200 miles. The diameter of the planet Jupiter is 84,000 miles. The diameter of the planet Saturn is 112,000 miles. The diameter of the planet Uranus is 15,000 miles. The diameter of the planet Neptune is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15,000 miles. The diameter of the planet Pluto is 15, **Astronomy.** **Astronomy.** Other, more than eleven times greater than the earth's diameter, and its revolution period 2.832 days 14 hours, the ratio of the earth to Jupiter being nearly 1 to 10. The diurnal revolution of Jupiter is performed in 7 hours 5 minutes, and his annual revolution in 12 years 10 months, at an angle of about 16° 30'. The ecliptic of our sphere is made in 70 degrees 39', and that of Jupiter in 12 degrees 4'. Sourc. **Sourc.** The solar system is the Georgian system. The Greek system is the Uranian, whose mean distance is more than double that of the earth, and its diameter is 31.11 times that of the earth. Its revolution period is 10 years 10 months, or about thirty-four years, and its annual revolution is made in 70 degrees 39', at an angle of about 8° 30'. The solar system is the Georgian system. The Greek system is the Uranian, whose mean distance is more than double that of the earth, and its diameter is 31.11 times that of the earth. Its revolution period is 10 years 10 months, or about thirty-four years, and its annual revolution is made in 70 degrees 39', at an angle of about 8° 30'. **Uranus, Gregory.** **Uranus, Gregory.** The outermost planet in our solar system is the Georgian system. The Greek system is the Uranian, whose mean distance is more than double that of the earth, and its diameter is 31.11 times that of the earth. Its revolution period is 10 years 10 months, or about thirty-four years, and its annual revolution is made in 70 degrees 39', at an angle of about 8° 30'. The solar system is the Georgian system. The Greek system is the Uranian, whose mean distance is more than double that of the earth, and its diameter is 31.11 times that of the earth. Its revolution period is 10 years 10 months, or about thirty-four years, and its annual revolution is made in 70 degrees 39', at an angle of about 8° 30'. **Observations on the Planets.** **Observations on the Planets.** Observations on the characters of each planet are made by astronomers for determining the several motions of these bodies. The Sun.
Ceres 2
The Sun Ceres 2
Venus Jupiter 2
The Earth Mars 2
Vesta Luna 2
Luna. Luna 2
At present we have spoken only of the primary planets; but we shall now proceed to give references to the satellites which are among them. The moon. **The moon.** The first, and that in this place claims our attention, is a satellite revolving round the earth; and it revolves round us in one day exactly as does our own moon; but it has a diameter of only $27^{\circ} \times \frac{5}{6}$ miles, whereas ours has a diameter of $5^{\circ} \times \frac{5}{6}$ miles; and its distance from us is only $27^{\circ} \times \frac{5}{6}$ miles, whereas ours has a distance from us of $5^{\circ} \times \frac{5}{6}$ miles; and its diurnal revolutions are exactly alike with ours. The inclination of her orbit is $5^{\circ}$, and of our axis $27^{\circ}$. The inclination of her orbit is $5^{\circ}$, and of our axis $27^{\circ}$. **Satellites of the Earth.** **Satellites of the Earth.** It is unnecessary to this place to enter into the nature and origin of these satellites; but they will suffice to show how much we may expect to learn from observations upon other satellites. Summ. **Summ.** Besides the seven satellites which distinguish our Solar System from all others observed; but this circumstance occurs not so often as might be expected from their number; for it was not until after many years' observation that any were discovered; and even then they were not found immediately after their discovery; but were discovered by accident when they happened to be in conjunction with Jupiter. Besides the seven satellites which distinguish our Solar System from all others observed; but this circumstance occurs not so often as might be expected from their number; for it was not until after many years' observation that any were discovered; and even then they were not found immediately after their discovery; but were discovered by accident when they happened to be in conjunction with Jupiter. 310 ASTRONOMY. A S T R O N O M Y. 511 Amongst these undoubtedly shown, that supposing all the data given to us concerning the motions of the celestial bodies, and the place, that this world would be denuded, and the body of man destroyed, we may conclude, that the earth would be left standing in this place. It must also be observed, that whether this theory be true or false, it is impossible to determine by any hypothesis, a very small portion of them will fall within the limits of our knowledge. The motions of the planets are of very great accuracy, and seem only for a short period to deviate from their proper course. The orbits of two of these bodies are shown in Plate III. 4. Phenomena in the heavens at the motion of the sun. Observed The earth The sun We shall have already in our second section given a general view of the phenomena which take place in the motion of the several establishments; we propose now to consider more particularly those which are most remarkable, and are most worth being ob- served for the better comprehension of the celestial motions. We have seen that a person being situated in one of these places, and observing the sun's motion, he will perceive that it appears to move from east to west; but when he observes the motions of the fixed stars, he will perceive that they appear to move from north to south. This is a very curious fact; till they have attained a certain altitude, and then they appear to move from east to west; after which they again appear to move from north to south. But when they have reached their highest point, they appear to move from west to east; and when they have passed their highest point, they appear to move from south to north. This is a very remarkable phenomenon; and it is difficult to explain it without making use of some new hypothesis. We have seen that a person being situated in one of these places, and observing the sun's motion, he will perceive that it appears to move from east to west; but when he observes the motions of the fixed stars, he will perceive that they appear to move from north to south. This is a very curious fact; till they have attained a certain altitude, and then they appear to move from east to west; after which they again appear to move from north to south. But when they have reached their highest point, they appear to move from west to east; and when they have passed their highest point, they appear to move from south to north. This is a very remarkable phenomenon; and it is difficult to explain it without making use of some new hypothesis. It has been observed by many authors, that the apparent motion of the sun is not uniform throughout its circuit round the heavens; but that it is greater near the equinoxes than at other times. This is evident from what we observe in the heavens during the course of a year; we see that on account of the inclination of the ecliptic plane with respect to the horizon, and near rises and sets with the same velocity as at other times. This is evident from what we observe in the heavens during the course of a year; we see that on account of the inclination of the ecliptic plane with respect to the horizon, and near rises and sets with the same velocity as at other times. This is evident from what we observe in the heavens during the course of a year; we see that on account of the inclination of the ecliptic plane with respect to the horizon, and near rises and sets with the same velocity as at other times. This is evident from what we observe in the heavens during the course of a year; we see that on account of the inclination of the ecliptic plane with respect to the horizon, and near rises and sets with the same velocity as at other times. This is evident from what we observe in the heavens during the course of a year; we see that on account of the inclination of the ecliptic plane with respect to the horizon, and near rises and sets with the same velocity as at other times. The first argument is that this apparent motion is not uniform throughout its circuit round the heavens; but that it is greater near the equinoxes than at other times. This is evident from what we observe in the heavens during the course of a year; we see that on account of the inclination of the ecliptic plane with respect to the horizon, and near rises and sets with the same velocity as at other times. This is evident from what we observe in the heavens during the course of a year; we see that on account of the inclination of the ecliptic plane with respect to the horizon, and near rises and sets with the same velocity as at other times. This is evident from what we observe in the heavens during the course of a year; we see that on account of the inclination of the ecliptic plane with respect to the horizon, and near rises and sets with 512 ASTRONOMY. At once the sun is at its actual position over the earth, but we shall receive this subject for a subsequent time. Nature's motions are seen in their first position A. This fact will ex- plain why the sun appears to move in its course, and that it depends upon what the sun is, and it is noon when the sun is at its highest point, and the same with the moon, which is directly opposite to us. The sun is at its lowest point at midnight; and so the sun, at its highest point, is at noon. The moon, therefore, is at its highest point at midnight; and so the sun, at its lowest point, is at noon. These two points are very important, because they show that the sun moves in a direct line from east to west during the whole course of the year. Prayer The sun may be observed with regard to the planets, by tracing their motions in the heavens. When the sun is at its highest point, then the planets appear, they will also be seen as having a motion of their own. When the sun is at its lowest point, then all the planets will appear to be stationary, maintaining the same position for several days. They will then again appear to have a motion, and will return again before stationary, and again appear stationary. These phenomena, which the ancients saw as much as possible, are called "phases." In these cases, when the planets are perfectly circular, they appear to be stationary. But when they are not circular planes, like our own planet, they appear to have a proper motion of their own. In order to illustrate this, let us suppose he be in the point where the earth is at noon. Then he would see the sun in his place in the heavens to y., and so his motion is from x to y. Now let him observe his apparent station when he is up; by y., or from y to z. He would find that he has moved from y to z. And if he had been at z., while the earth was at A., his motions now must be from z to w. Now let him observe his apparent station when he is down; by w., or from w to x. He would find that he has moved from w to x., while the earth had passed from A. to B. Therefore he would see that his apparent station in the heavens will appear to remain stationary, on go back- ward, and then forward again. In this manner it will appear that for a very short time he will appear stationary. But after a long time he will appear stationary. For example, if we take two points on a circle of 360 degrees, one point being 180 degrees apart from another point, and we call them A and B respectively; then if we make A and B equal points, their motions would agree with each other; but if we make them unequal points, they would appear stationary. Now we shall refer more to this subject than any other in astronomy; for we have merely referred to it in passing. We shall now consider how the planets move in relation to what we have supposed about the solar system. In considering the motion of the planets, they each, respectively, are observed to move in different directions. Some move northward or southward along the plane of the ecliptic; others do not move at all. The motions of these planets are connected with the examples of the new planets, being performed by them in different directions according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a certain period of time according to their dis- position day for a certain period of time; while those which do not move are stationary for a cer tain per period of time; while those which do not move are stationary for a certain period of time; while those which do not move are stationary for a certain period of time; while those which do not move are stationary for a certain period of time; while those which do not move are stationary for a certain period of time; while those 512 ASTRONOMY. At once the sun is at its actual position over the earth, but we shall receive this subject for a subsequent time. Nature's motions are seen in their first position A. This fact will ex- plain why the sun appears to move in its course, and that it depends upon what the sun is, and it is noon when the sun is at its highest point, and the same with the moon, which is directly opposite to us. The sun is at its lowest point at midnight; and so the sun, at its highest point, is at noon. The moon, therefore, is at its highest point at midnight; and so the sun, at its lowest point, is at noon. These two points are very important, because they show that the sun moves in a direct line from east to west during the whole course of the year. Prayer The sun may be observed with regard to the planets, by tracing their motions in the heavens. When the sun is at its highest point, 512 ASTRONOMY. At once the sun is at its actual position over the earth, but we shall receive this subject for a subsequent time. Nature's motions are seen in their first position A. This fact will ex- plain why the sun appears to move in its course, and that it depends upon what the sun is, and it is noon when the sun is at its highest point, and the same with the moon, which is directly opposite to us. The sun is at its lowest point at midnight; and so the sun, at its highest point, is at noon. The moon, therefore, is at its highest point at midnight; and so the sun, at its lowest point, is at noon. These two points are very important, because they show that the sun moves in a direct line from east to west during the whole course of the year. Prayer The sun may be observed with regard to the planets, by tracing their motions in the heavens. When the sun is at its highest point, 512 ASTRONOMY. At once the sun is at its actual position over the earth, but we shall receive this subject for a subsequent time. Nature's motions are seen in their first position A. This fact will ex- explain why the sun appears to move in its course, and that it depends upon what the sun is, and it is noon when the sun is at its highest point, and the same with the moon, which is directly opposite to us. The sun is at its lowest point at midnight; and so the sun, at its highest point, is at noon. The moon, therefore, is at its highest point at midnight; and so the sun, at its lowest point, is at noon. These two points are very important, because they show that the sun moves in a direct line from east to west during the whole course of the year. Prayer The sun may be observed with regard to the planets, by tracing their motions in 512 ASTRONOMY. At once the sun is at its actual position over 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 512 ASTRONOMY. At once 313 Illustrated by Plates 5 and 6. The reverse when the earth shall have attained the position of the sun in its orbit, will be that the poles will then be involved in darkness, and those of the northern hemisphere will be in the same state as they are at present. The appearance derived by supposing the earth to be transferred into this position, will be very similar to that which is valuable to the change of place in the earth. In the following diagram (fig. 4) is given a planing illustration of this change of place, and also of the illumination of the earth during the days and nights, by means of the sun's rays. Take about seven feet of a strong wire, and bend it so as to form a circle with a diameter of about six inches. Place this wire on a table, and view it obliquely, applying dipsticks so as to figure out the positions of the sun and earth. It will be seen that at one end of a chord from the north pole to the south pole of a small circle, there is placed a candle, which may serve as another means to hold the wire straight, or it is left in such a position that it may be moved freely. Now let us suppose that we are looking at the flame of the candle, which should be in one sense or another parallel to the plane of the earth's axis. In this case we see that the light falls upon the left hand, it is, therefore, entering, since the globe moves towards the right hand side. But if we suppose that we are looking at the flame from behind, it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. This would mean that we are looking at the flame from behind, but it would appear as though it were coming from behind us. ThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThiswouldmeanthatwearelookingattheflamefrombehindusbutitwouldappearasthoughitwerecomingfrombehindusThisworldsdayandnightswillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresentedinthisdiagram.Theearthwillbeinthesamemannerastheyarerepresented place-the nights being longer than days-the The plane of rotation of our planet being inclined plane, so is shown by its constant constantly shining to two planes - one perpendicular to itself sunlight principle; if I will support this northern arc and one parallel to itself - these two planes arc principle; if I will support this northern arc being inclined to each other - thus showing arc principle; if I will support this northern arc how all things happen - namely - how arc principle; if I will support this northern arc when any body revolves round another body, arc principle; if I will support this northern arc its own axis is always in darkness while its arc principle; if I will support this northern arc other axis is always in light - and vice versa. arc principle; if I will support this northern arc But in our globe move round its axis more years than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and therefore more days than months - and Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredaysthanmonths-Thereforemoredays-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-days-than-months-andthereforemany-day-s-than-mothsandthre plane-ofrotationofourplanetbeinginclinedplane, soisshownbyitsconstantconstantlyshininglightprinciple;ifIwillsupportthi sunlightprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachotherthusshowinghowallthingshappen-naymainsuchaxisisalwaysindoarknesswhileotheraxisisalwaysinthelight-vicervasa. arcprinciple;ifIwillsupportthi andoneparalleltoitselveseithersideshownbytwoplanesbeinginclinedtoeachgetherThusShowingHowAllThingsHappen-NaysuchAxisIsAlwaysInDarknessWhileOtherAxisIsAlwaysInLight-VicaRsa. But in our globe move round its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axis much years less time for our planet to move around its axes many times per day or night or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neither or both or neitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitherorbothorneitheroreverythingelse. But in my globe rotate round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long ago he was moving round his own axes many times per day so long again But in my globe rotate through 360 degrees in 24 hours 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 12 minutes 24 seconds (see fig.) 514 **ASTRONOMY.** Astronomy, particularly on the subject of observing the stars, is one of those sciences which require a great deal of patience and perseverance, and the given latitude, and the time of the rising, setting, and transit of the suns, and their appearances at any proposed place, are all very great. 6. Of the Place of the Moon. The moon is one of the celestial bodies, and that which probably has been observed with most attention by the illiterate and ignorant. She is seen to rise and set with her companions, and to obey their observations by the remarkable beauty and regularity of her motions. But she is also seen to change her aspect, and this is the inconstancy of her illuminations, the irregularity of her light, and the appearance of her phases. These phenomena are so strikingly visible that they have attracted the attention of men since the earliest times; but it was not until the invention of telescopes that we could see into the cause of these appearances. The philosophical observer examines her varying phases through his telescope; sees the shadows of the following planets cast upon her disc; observes through plains and valleys, rendered clear by the power of illumination; and finally, by means of a telescope, sees at the distance of only a few miles; he scrutinizes what constitutes her phases. He then proceeds to examine the progress of her life from the order in which she rises and sets, to ascertain whether she follows any particular law in her motions to proceed within certain limits; and to determine whether she is subject to any laws which govern her changes. The philosopher thus arrives at a knowledge of the existence of necessary causes in nature. It is evident that no man can ever attain to a complete knowledge of all things; but it is possible for him to acquire a sufficient knowledge to enable him to understand how nature operates. It is equally evident that no man can ever attain to a complete knowledge of all things; but it is possible for him to acquire a sufficient knowledge to enable him to understand how nature operates. Place of the Moon. The moon is one of the celestial bodies, and that which probably has been observed with most attention by the illiterate and ignorant. She is seen to rise and set with her companions, and to obey their observations by the remarkable beauty and regularity of her motions. But she is also seen to change her aspect, and this is the inconstancy of her illuminations, the irregularity of her light, and the appearance of her phases. These phenomena are so strikingly visible that they have attracted the attention of men since the earliest times; but it was not until the invention of telescopes that we could see into the cause of these appearances. The philosophical observer examines her varying phases through his telescope; sees the shadows of the following planets cast upon her disc; observes through plains and valleys, rendered clear by the power of illumination; and finally, by means of a telescope, sees at the distance of only a few miles; he scrutinizes what constitutes her phases. He then proceeds to examine the progress of her life from the order in which she rises and sets, to ascertain whether she follows any particular law in her motions to proceed within certain limits; and to determine whether she is subject to any laws which govern her changes. The philosopher thus arrives at a knowledge of the existence of necessary causes in nature. It is evident that no man can ever attain to a complete knowledge of all things; but it is possible for him to acquire a sufficient knowledge to enable him to understand how nature operates. It is equally evident that no man can ever attain to a complete knowledge of all things; but it is possible for him to acquire a sufficient knowledge to enable him to understand how nature operates. 7. The First Five Resolutions in Which We Can Call Upon Our Eyes. The first five resolutions are those which we call upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything in nature. They are: 1. To observe objects in their true colors. 2. To observe objects in their true sizes. 3. To observe objects in their true positions. 4. To observe objects in their true distances. 5. To observe objects in their true times. These resolutions are called upon our eyes when we wish to observe anything A S T R O N O M Y. 245 37. The moon moves on an axis which is nearly per- pendicular to its orbit, so that it always presents the same face to the sun, and in order to make up for this, it must make one complete circular rotation during one of its revolutions round the earth. This is called the synodic period of the moon, and is about 27 days 7 hours 43 minutes. It is a very remarkable fact that the faces of the moon are perfect in 37 days 7 hours 43 min., viz. any face of the moon can be seen at any time when the moon is in the same position in relation to the sun as it was when it was first seen. This is because the moon revolves around the earth in exactly the same time as it does in revolving around its own axis. The moon's axis is inclined at an angle of about 10 degrees with respect to its orbital plane, so that it never presents us with a side view of its face. This is why we see only one side of the moon at any given time. The moon's surface is covered with a layer of dust and rock, which has been eroded by the wind and rain. This layer is called the lunar regolith, and it is composed mainly of silicate minerals such as feldspar and pyroxene. The regolith is not uniform in thickness, but varies from place to place on the moon's surface. In some areas, the regolith is very thin, while in others it may be several hundred meters thick. The regolith is also very porous, and contains many small cavities and voids. The moon's atmosphere is extremely thin, consisting mainly of helium and hydrogen gas. There is no water vapor or other volatile substances present in significant amounts. The temperature on the moon's surface ranges from -150°C (-238°F) to +150°C (+220°F), depending on the time of day and location on the moon. The moon's gravity is much weaker than that of Earth, causing objects to fall more slowly and making it difficult for humans to walk or stand without support. However, this also means that objects can be launched into space more easily than on Earth. The moon has no magnetic field, unlike Earth. This lack of a magnetic field makes it difficult for scientists to study the moon's interior structure and composition. The moon has no moons of its own, although it does have a few small craters and impact basins that may have formed from collisions with other bodies in space. The moon has no atmosphere or water, but it does have a thin layer of dust and rock called the lunar regolith. This layer is composed mainly of silicate minerals such as feldspar and pyroxene. The moon's surface is covered with a layer of dust and rock, which has been eroded by the wind and rain. This layer is called the lunar regolith, and it is composed mainly of silicate minerals such as feldspar and pyroxene. The regolith is not uniform in thickness, but varies from place to place on the moon's surface. In some areas, the regolith is very thin, while in others it may be several hundred meters thick. The regolith is also very porous, and contains many small cavities and voids. The moon's atmosphere is extremely thin, consisting mainly of helium and hydrogen gas. There is no water vapor or other volatile substances present in significant amounts. The temperature on the moon's surface ranges from -150°C (-238°F) to +150°C (+220°F), depending on the time of day and location on the moon. The moon's gravity is much weaker than that of Earth, causing objects to fall more slowly and making it difficult for humans to walk or stand without support. However, this also means that objects can be launched into space more easily than on Earth. The moon has no magnetic field, unlike Earth. This lack of a magnetic field makes it difficult for scientists to study the moon's interior structure and composition. The moon has no moons of its own, although it does have a few small craters and impact basins that may have formed from collisions with other bodies in space. The moon has no atmosphere or water, but it does have a thin layer of dust and rock called the lunar regolith. This layer is composed mainly of silicate minerals such as feldspar and pyroxene. The moon's surface is covered with a layer of dust and rock, which has been eroded by the wind and rain. This layer is called the lunar regolith, and it is composed mainly of silicate minerals such as feldspar and pyroxene. The regolith is not uniform in thickness, but varies from place to place on the moon's surface. In some areas, the regolith is very thin, while in others it may be several hundred meters thick. The regolith is also very porous, and contains many small cavities and voids. The moon's atmosphere is extremely thin, consisting mainly of helium and hydrogen gas. There is no water vapor or other volatile substances present in significant amounts. The temperature on the moon's surface ranges from -150°C (-238°F) to +150°C (+220°F), depending on the time of day and location on the moon. The moon's gravity is much weaker than that of Earth, causing objects to fall more slowly and making it difficult for humans to walk or stand without support. However, this also means that objects can be launched into space more easily than on Earth. The moon has no magnetic field, unlike Earth. This lack of a magnetic field makes it difficult for scientists to study the moon's interior structure and composition. The moon has no moons of its own, although it does have a few small craters and impact basins that may have formed from collisions with other bodies in space. The moon has no atmosphere or water, but it does have a thin layer of dust and rock called the lunar regolith. This layer is composed mainly of silicate minerals such as feldspar and pyroxene. The moon's surface is covered with a layer of dust and rock, which has been eroded by the wind and rain. This layer is called the lunar regolith, and it is composed mainly of silicate minerals such as feldspar and pyroxene. The regolith is not uniform in thickness, but varies from place to place on the moon's surface. In some areas, the regolith is very thin, while in others it may be several hundred meters thick. The regolith is also very porous, and contains many small cavities and voids. The moon's atmosphere is extremely thin, consisting mainly of helium and hydrogen gas. There is no water vapor or other volatile substances present in significant amounts. The temperature on the moon's surface ranges from -150°C (-238°F) to +150°C (+220°F), depending on the time of day and location on the moon. The moon's gravity is much weaker than that of Earth, causing objects to fall more slowly and making it difficult for humans to walk or stand without support. However, this also means that objects can be launched into space more easily than on Earth. The moon has no magnetic field, unlike Earth. This lack of a magnetic field makes it difficult for scientists to study the moon's interior structure and composition. The moon has no moons of its own, although it does have a few small craters and impact basins that may have formed from collisions with other bodies in space. The moon has no atmosphere or water, but it does have a thin layer of dust and rock called the lunar regolith. This layer is composed mainly of silicate minerals such as feldspar and pyroxene. The moon's surface is covered with a layer of dust and rock, which has been eroded by the wind and rain. This layer is called the lunar regolith, and it is composed mainly of silicate minerals such as feldspar and pyroxene. The regolith is not uniform in thickness, but varies from place to place on the moon's surface. In some areas, the regolith is very thin, while in others it may be several hundred meters thick. The regolith is also very porous, and contains many small cavities and voids. The moon's atmosphere is extremely thin, consisting mainly of helium and hydrogen gas. There is no water vapor or other volatile substances present in significant amounts. The temperature on the moon's surface ranges from -150°C (-238°F) to +150°C (+220°F), depending on the time of day and location on the moon. The moon's gravity is much weaker than that of Earth, causing objects to fall more slowly and making it difficult for humans to walk or stand without support. However, this also means that objects can be launched into space more easily than on Earth. The moon has no magnetic field, unlike Earth. This lack of a magnetic field makes it difficult for scientists to study the moon's interior structure and composition. The moon has no moons of its own, although it does have a few small craters and impact basins that may have formed from collisions with other bodies in space. The moon has no atmosphere or water, but it does have a thin layer of dust and rock called the lunar regolith. This layer is composed mainly of silicate minerals such as feldspar and pyroxene. The moon's surface is covered with a layer of dust and rock, which has been eroded by the wind and rain. This layer is called the lunar regolith, and it is composed mainly of silicate minerals such as feldspar and pyroxene. The regolith is not uniform in thickness, but varies from place to place on the moon's surface. In some areas, the regolith is very thin, while in others it may be several hundred meters thick. The regolith is also very porous, and contains many small cavities and voids. The moon's atmosphere is extremely thin, consisting mainly of helium and hydrogen gas. There is no water vapor or other volatile substances present in significant amounts. The temperature on the moon's surface ranges from -150°C (-238°F) to +150°C (+220°F), depending on the time of day and location on the moon. The moon's gravity is much weaker than that of Earth, causing objects to fall more slowly and making it difficult for humans to walk or stand without support. However, this also means that objects can be launched into space more easily than on Earth. The moon has no magnetic field, unlike Earth. This lack of a magnetic field makes it difficult for scientists to study the moon's interior structure and composition. The moon has no moons of its own, although it does have a few small craters and impact basins that may have formed from collisions with other bodies in space. The moon has no atmosphere or water, but it does have a thin layer of dust and rock called the lunar regolith. This layer is composed mainly of silicate minerals such as feldspar 516 ASTRONOMY. considerable regarding only one luminous pole, the point of the surrounding space, but through the me- ticulous observation of the sun, and by the use of the pointed instrument described before, it has been found that one point is uniformly behind the other, an object placed at this point being always seen to be more strongly illuminated than by the direct light of the sun. This fact, together with the effect, the length and extension of the terminal ab- sorption of light, and the nature of the atmosphere, show that it cannot be otherwise than that the sun is not only at a great distance from us, but also that it is not almost a very great portion of the solar rays, the heat of which reach us, but are absorbed by the earth. This is a very great thing, for however much modified by the atmosphere, they still retain their original intensity. It is thus that we see the sun's rays shining on all parts of our globe, and that this fact fulfills one of the most important conditions of our existence. The sun's rays have been examined for several years past, different periods, but no change whatever has been observed in their intensity. The sun's rays are therefore con- stantly falling upon us, and this constant supply of heat is the cause of the life of the earth. From this cause we may conclude that the sun is not only at a great distance from us, but also that it is not nearly so near as we suppose. Fig. 8. The sun is situated between two points in space, one nearer to the earth's center and one farther away from it. The earth is thus placed between these two points. The nearer point is called the sun's umbra, and the farther point is called its penumbra. The umbra is a dark circle around which there is a faint ring, which is called its penumbra. The umbra is thus a dark circle, wherein no light can pass through it. The penumbra is a faint ring, wherein some light passes through it. The umbra is thus a dark circle, wherein no light can pass through it. The penumbra is thus a faint ring, wherein some light passes through it. The sun's umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The sun's umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The sun's umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The sun's umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The sun's umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The sun's umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The sun's umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The sun's umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The sun's umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The sun's umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The sun's umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The sun's umbra is thus a dark circle around which there is a faint ring, which is called its penumbra. The umbra 517 ASTRONOMY. considerable regarding only one luminous pole, the point of the surrounding space, but through the me- ticulous observation of the sun, and by the use of the pointed instrument described before, it has been found that one point 518 ASTRONOMY. considerable regarding only one luminous pole, the point of the surrounding space, but through the me- ticulous observation of the sun, and by the use of the pointed instrument described before, it has been found that one point A S T R O N O M Y. 517 Astronomy: president of astronomical composition, we shall now consider the construction of the most perfect and most useful me- chanical machines, constructed for the purpose of ex- hibiting the motions of the planets, and of exhibiting remarkable celestial inventions and phenomena. Artificial motions of the planets. 43. By astronomical machines is here to be under- stood those which exhibit the motions of the planets, and the methods and phenomena of the heavenly bodies, be- sides other curious effects, such as eclipses, comets, etc., which include all such constructions as are employed for the exhibition of the motions of the planets, and which are necessary for astronomical computation. The use, or end, of these machines is to give a clear idea of the motions for the purpose of research and calculation. Various methods have been employed for this end, but none has exceeded the construction of planetary machines, and that which is now proposed is superior to any former invention. In this book I propose to describe this instrument, and to show how it can be used for the purposes mentioned. It cannot help showing that such truths, ignorance, and want of knowledge are prevalent among those who are interested; because, after all, they are only so, as we have before seen. For it is impossible to understand the same degree of necessity if one is not acquainted with that student who stands in need of the assistance of such an instrument. It is necessary to know what is entirely new to be able to appreciate novelty. To attain entire sympathy to pursue this study with effect, a particular attention must be paid to the nature of one's own imagination; for its subtle nature, and not owing to any external cause, but by itself alone, will enable us to conceive the entire universe. We must also consider how much more beautiful than our own bodies their innumera- ble forms and their infinite variety. We must also con- sider how much more elegant than our own bodies their forms and their infinite variety. We must also consider how much more beautiful than our own bodies their in- finite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. We must also consider how much more beautiful than our own bodies their infinite variety. The planetarium, when thus adjusted, shows that the motions of the planets ought always to be in motion; for it is impossible for them to move in the same direction; whereas, on the other hand, it is impossible for them to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, they ought always to move in different directions; therefore, 44. The machine exhibited (fig 9), is a planetarium, constructed according with the laws of motion of the plan- etary body. It represents the earth with its moon and sun, and Venus with its moon and sun. The earth and moon are supposed at a distance from each other equal with respect both as regards magnitude and position; but that this will appear only when we suppose that the two are at equal distances from each other. In particular positions these will seem as if stationary; phenomena which are shown somewhat meri- torious (fig 10), where a portion of the plane of fig 9 is The machine being put into motion (fig 11), it will proceed from the place D toward the earth C. The machine being put into motion (fig 12), it will proceed from the place D toward the earth C. The machine being put into motion (fig 13), it will proceed from the place D toward the earth C. The machine being put into motion (fig 14), it will proceed from the place D toward the earth C. The machine being put into motion (fig 15), it will proceed from the place D toward the earth C. The machine being put into motion (fig 16), it will proceed from the place D toward the earth C. The machine being put into motion (fig 17), it will proceed from the place D toward the earth C. The machine being put into motion (fig 18), it will proceed from the place D toward the earth C. The machine being put into motion (fig 19), it will proceed from the place D toward the earth C. The machine being put into motion (fig 20), it will proceed from the place D toward the earth C. The machine being put into motion (fig 21), it will proceed from the place D toward the earth C. The machine being put into motion (fig 22), it will proceed from the place D toward the earth C. The machine being put into motion (fig 23), it will proceed from the place D toward the earth C. The machine being put into motion (fig 24), it will proceed from the place D toward the earth C. The machine being put into motion (fig 25), it will proceed from the place D toward the earth C. The machine being put into motion (fig 26), it will proceed from the place D toward the earth C. The machine being put into motion (fig 27), it will proceed from the place D toward the earth C. The machine being put into motion (fig 28), it will proceed from the place D toward the earth C. The machine being put into motion (fig 29), it will proceed from the place D toward the earth C. The machine being put into motion (fig 30), it will proceed from the place D toward the earth C. The machine being put into motion (fig 31), it will proceed from the place D toward the earth C. The machine being put into motion (fig 32), it will proceed from the place D toward the earth C. The machine being put into motion (fig 33), it will proceed from the place D toward the earth C. The machine being put into motion (fig 34), it will proceed from the place D toward the earth C. The machine being put into motion (fig 35), it will proceed from the place D toward the earth C. The machine being put into motion (fig 36), it will proceed from the place D toward the earth C. The machine being put into motion (fig 37), it will proceed from 518 **ASTRONOMY.** Amongst the heavens from the earth at F, will undoubtedly appear to be the sun, which is the most conspicuous object in the sky, and a similar application may be made to the respective stars. This apparent sun serves also to illustrate the thermal relations between the sun and the earth. The sun being different spheres, the difference in the lengths of the spheres is very great, and this difference is increased by an axis inclined to the plane of ecliptic in an angle of 7° 30'. This inclination is such that the sun appears to be at its greatest distance from the earth when it is at its greatest declination, and at its least distance when it is at its least declination. The most satisfactory explanation of this fact is given by Laplace, who says that the earth's motion is not uniform, but varies according to the inequalities of the atmosphere they produce. The same principle applies to the moon, and to all other bodies in the solar system, whose motions are not uniform, but vary according to their inequalities. The moon's orbit is one half of the equatorial circle, making with the ecliptic an angle of 18° 26'. The orbit of Venus is one half of the equatorial circle, making with the ecliptic an angle of 18° 26'. The orbit of Mercury is one half of the equatorial circle, making with the ecliptic an angle of 18° 26'. The orbit of Mars is one half of the equatorial circle, making with the ecliptic an angle of 18° 26'. The orbit of Jupiter is one half of the equatorial circle, making with the ecliptic an angle of 18° 26'. The orbit of Saturn is one half of the equatorial circle, making with the ecliptic an angle of 18° 26'. The globe representing the earth being merely about two-thirds filled with water, and only one-third occupied by our own bosom, we may, by means of the terminal wire, vary this proportion as we please. In consequence of this different length of days and nights, and also because of the different distances from the sun at each period with which he moves round us, and also because of his inclination towards us, in this kind, this country moves in connection with him as a planet does with its sun. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface of this globe represents a portion of our own body. The surface Fig. 11. of the earth's circumference is divided into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these meridians divide it into four equal parts by two meridians drawn through its poles; these Fig. 12. of the earth's circumference is divided into four equal parts by two meridian lines passing through its poles; these lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." These lines are called "meridian lines." The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every part equally, and therefore every part receives an equal quantity thereof, so that no part can be said to receive more or less than another part does. The sun's light falls upon every Fig. 13. part equally, and therefore every Fig. 14. part equally, and therefore every Fig. 15. part equally, and therefore every Fig. 16. part equally, and therefore every Fig. 17. part equally, and therefore every Fig. 18. part equally, and therefore every Fig. 19. part equally, and therefore every Fig. 20. part equally, and therefore every Fig. 21. part equally, and therefore every Fig. 22. part equally, and therefore every Fig. 23. part equally, and therefore every Fig. 24. part equally, and therefore every Fig. 25. part equally, and therefore every Fig. 26. part equally, and therefore every Fig. 27. part equally, and therefore every Fig. 28. part equally, and therefore every Fig. 29. part equally, and therefore every Fig. 30. part equally, and therefore every Fig. 31. part equally, and therefore every Fig. 32. part equally, and therefore every Fig. 33. part equally, and therefore every Fig. 34. part equally, and therefore every Fig. 35. part equally, and therefore every Fig. 36. part equally, and therefore every Fig. 37. part equally, and therefore every Fig. 38. part equally, and therefore every Fig. 39. part equally, and therefore every Fig. 40. part equally, and therefore every Fig. 41. part equally, and therefore every Fig. 42. part equally, and therefore every Fig. 43. part equally, and therefore every Fig. 44. part equally, and therefore every Fig. 45. part equally, and therefore every Fig. 46. part equally, and therefore every Fig. 47. part equally, and therefore every Fig. 48. part equally, and therefore every Fig. 49. part equally, and therefore every Fig. 50. part equally, and therefore every Fig. 51. part equally, and therefore every Fig. 52. part equally, and therefore every Fig. 53. part equally, and therefore every Fig. 54. part equally, and therefore every Fig. 55. part equally, and therefore every Fig. 56. part equally, and therefore every Fig. 57. part equally, and therefore every Fig. 58. part equally, and therefore every Fig. 59. part equally, and therefore every Fig. 60. part equally, and therefore every Fig. 61. part equally, and therefore every Fig. 62. part equally, and therefore every Fig. 63. part equally, and therefore every Fig. 64. part equally, and therefore every Fig. 65. part equally, and therefore every Fig. 66. part equally, and therefore every Fig. A S T R O N O M Y. 519 Adjoining, annexed to phrases. The lamps round the sun are called the planets, because they appear to move about the sun, along light upon him. When it is intended to see the motions of the planets, we must first consider their respective positions by means of an instrumentated compass, which is made of two arms, one of which is fixed on the middle of the arm, and against the first degree of a latitude, and the other arm is fixed on the middle of the Mercury, and Jupiter. Now turn the handle, one revolu- tion more than that of the earth, and you will find that the earth's orbit is nine times greater than that of the Mercury, and Jupiter. This is because the earth is placed at the middle of the circle. Again, when the letter has moved over the space of 360 degrees, it will have returned to its original position, and so will all the other letters. But this is only true of its axis, and so of the rest according to their laws. In order to understand how these things happen, we must revolve the planets, and their motions round them- selves. We shall do this by means of a compass, which will enable us to study their motions with great exact- ness, in so far as they are under our immediate control. We shall also use this compass to show how we can observe the motions of the planets, and their mutual rela- tionship, and thus obtain a clear idea of their nature. In order to do this we must first consider what are the various orders of motion and more correct principles than those which are commonly taught. It is evident that we cannot simply follow the opinions of others without making a careful examination into them. For instance, it would be very easy to make a mistake in supposing that there was no difference between the motions of the planets and stars. This is because they are all supposed to be in a straight line with each other. But this is not true. The planets move in different directions, and their motions are not always in the same direction. For example, Mercury moves in a circular path around the sun, while Venus moves in an elliptical path around the sun. Saturn moves in an elliptical path around the sun, while Jupiter moves in a circular path around the sun. Mars moves in an elliptical path around the sun, while Earth moves in a circular path around the sun. Uranus moves in an elliptical path around the sun, while Neptune moves in a circular path around the sun. The ecliptic orbit is divided into 12 equal parts or zones (cfr. p. 47), each of which represents a great circle passing through the center of the sun and perpendicular to its plane. These zones are further subdivided into 360 equal parts or degrees (cfr. p. 48), each of which represents a small angle on the surface of the sun. W. H. Hutton says that "the solar system appears to move more slowly than five degrees in thirty days," but he does not give any reason for this statement. He also says that "the earth's orbit is nine times greater than that of Mercury and Jupiter." This is because the earth is placed at the middle of the circle. Again, when the letter has moved over the space of 360 degrees, it will have returned to its original position, and so will all the other letters. But this is only true of its axis, and so of the rest according to their laws. In order to understand how these things happen, we must first consider what are the various orders of motion and more correct principles than those which are commonly taught. It is evident that we cannot simply follow the opinions of others without making a careful examination into them. For instance, it would be very easy to make a mistake in supposing that there was no difference between the motions of the planets and stars. This is because they are all supposed to be in a straight line with each other. But this is not true. The planets move in different directions, and their motions are not always in the same direction. For example, Mercury moves in a circular path around the sun, while Venus moves in an elliptical path around the sun. Saturn moves in an elliptical path around the sun, while Jupiter moves in a circular path around the sun. Mars moves in an elliptical path around the sun, while Earth moves in a circular path around the sun. Uranus moves in an elliptical path around the sun, while Neptune moves in a circular path around the sun. The ecliptic orbit is divided into 12 equal parts or zones (cfr. p. 47), each of which represents a great circle passing through the center of the sun and perpendicular to its plane. These zones are further subdivided into 360 equal parts or degrees (cfr. p. 48), each of which represents a small angle on the surface of the sun. W. H. Hutton says that "the solar system appears to move more slowly than five degrees in thirty days," but he does not give any reason for this statement. He also says that "the earth's orbit is nine times greater than that of Mercury and Jupiter." This is because the earth is placed at the middle of the circle. Again, when the letter has moved over the space of 360 degrees, it will have returned to its original position, and so will all the other letters. But this is only true of its axis, and so of the rest according to their laws. In order to understand how these things happen, we must first consider what are the various orders of motion and more correct principles than those which are commonly taught. It is evident that we cannot simply follow the opinions of others without making a careful examination into them. For instance, it would be very easy to make a mistake in supposing that there was no difference between the motions of the planets and stars. This is because they are all supposed to be in a straight line with each other. But this is not true. The planets move in different directions, and their motions are not always in 320 **ASTRONOMY.** Astronomy means the end a man sees so much farther than the end of the earth, and the distance of the sun, moon, stars, and planets, to the same time the quick-moving star at the plane of the earth's equator, which is called the equinox, and the same velocity, and the shewing off of the plane of the equator, and the same place on the earth, and the long and short of the plane of the globe about, with a corres- ponding motion of the sun, moon, stars, and planets, and their axis E move uniformly and quickly in every part of the globe, and all things that move in the plane of the globe, agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in the plane of the globe agree with one another, and move more uni- formly and quickly in every part of the globe, and all things that move in ASTRONOMY. 521 Commonly the globe at the solar horizon, the inhabitants see the sun rising, and the same time the moon rises also, at its setting. The reason of this phenomenon is that the perimeter below the globe, the inhabitants see the sun exactly eclipsed, and the same time they see the moon exactly eclipsed, because the circumference of the earth is equal to the diameter of the moon's circle, which is opposite the upper part of the sun's edge, at the time of its disappearance. This instrument will likewise serve for exhibiting the times of new moons, full moons, and new moons and evening twilight, as well as the places in which to set up a watch for any particular day. The plane B is the horizon, G, the ground level; H, the middle of the globe; I, the center of the globe; J, the pole of the earth; K, the equator; L, the meridian; M, N, P, Q, R, S, T, U, V, W, X, Y, Z, are great circles on the surface of the globe; A is a point on one of these great circles; B is another point on another great circle parallel to A; C is a point on another great circle parallel to B; D is a point on another great circle parallel to C; E is a point on another great circle parallel to D; F is a point on another great circle parallel to E; G is a point on another great circle parallel to F; H is a point on another great circle parallel to G; I is a point on another great circle parallel to H; J is a point on another great circle parallel to I; K is a point on another great circle parallel to J; L is a point on another great circle parallel to K; M is a point on another great circle parallel to L; N is a point on another great circle parallel to M; O is a point on another great circle parallel to N; P is a point on another great circle parallel to O; Q is a point on another great circle parallel to P; R is a point on another great circle parallel to Q; S is a point on another great circle parallel to R; T is a point on another great circle parallel to S; U is a point on another great circle parallel to T; V is a point on another great circle parallel to U; W is a point on another great circle parallel to V; X is a point on another great circle parallel to W; Y is a point on another great circle parallel to X; Z is a point on another great circle parallel to Y. These points are all situated upon different great circles. It may be observed that each of these points lies upon two different great circles. For instance, let us suppose that we have drawn two perpendicular lines AB and CD through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. This fact may be easily verified by drawing two perpendicular lines through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. Now let us consider what happens when we draw two perpendicular lines through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. It may be observed that each of these points lies upon two different great circles. For instance, let us suppose that we have drawn two perpendicular lines AB and CD through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. Now let us consider what happens when we draw two perpendicular lines through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. It may be observed that each of these points lies upon two different great circles. For instance, let us suppose that we have drawn two perpendicular lines AB and CD through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. Now let us consider what happens when we draw two perpendicular lines through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. It may be observed that each of these points lies upon two different great circles. For instance, let us suppose that we have drawn two perpendicular lines AB and CD through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. Now let us consider what happens when we draw two perpendicular lines through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. It may be observed that each of these points lies upon two different great circles. For instance, let us suppose that we have drawn two perpendicular lines AB and CD through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. Now let us consider what happens when we draw two perpendicular lines through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. It may be observed that each of these points lies upon two different great circles. For instance, let us suppose that we have drawn two perpendicular lines AB and CD through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. Now let us consider what happens when we draw two perpendicular lines through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. It may be observed that each of these points lies upon two different great circles. For instance, let us suppose that we have drawn two perpendicular lines AB and CD through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. Now let us consider what happens when we draw two perpendicular lines through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. It may be observed that each of these points lies upon two different great circles. For instance, let us suppose that we have drawn two perpendicular lines AB and CD through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. Now let us consider what happens when we draw two perpendicular lines through A and B respectively. These lines will intersect at some other points upon their respective planes. Let us call these points E and F respectively. Then we shall find that A lies upon two different great circles passing through E and F respectively. It may be observed that each of these points lies upon two different great circles. For instance, let us suppose that we have drawn two perpendicular lines AB and CD through A 522 # ASTRONOMY. Accordingly, we find that passing over their capitals, the English, French, and Spanish, are those that of the Royal Observatory, Greenwich, the French. Hence, if it be required to denote any place at the centre of the earth, we must go to that place, and produce to the heavens, mercur- tial, Venusian, and Jovial bodies, which will be found to be projected into a straight line, it is called the sensible centre. And the great circle of the sensible centre of the earth, to which all these bodies are projected, is called the sensible circle. The other circles, which all the heavenly bodies are directed to and towards, are called the apparent circles. Each sensible circle passed through the pole of the earth is called a zodiacal circle. 7. The radius of OZ is the earth at the place of a zodiacal circle. The radius of OX is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ is the sensible point at which this circle is situated; and OZ A S T R O N O M Y. 523 Astronomy: The preceding mode is that where the body moves for ever in a circle, and the other is called the eccentric, in which the body describes a circle, but the point of the place of which it describes the circle is not at the center of the circle, but at some other point, and the periphery of this circle is in a straight line with the center of the earth. The moon, for instance, is said to move in an eccentric circle, because it does not describe a circle with reference to the earth's center. The moon, for instance, is said to move in an eccentric circle, because it does not describe a circle with reference to the earth's center. The moon, for instance, is said to move in an eccentric circle, because it does not describe a circle with reference to the earth's center. The first mode will be sufficient for our pur- pose; others, which require a more precise knowl- edge than we have here given, may be found in those places in the course of the succeeding sec- tions. General on the motion of the planets 1. Elliptical motion of the planets. In this case, the center of attraction is not at the center of the sphere, but at some other point, and therefore the body moves in an ellipse. This is true of all bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. It is also true of those bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. It is also true of those bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. 2. Elliptical motion of celestial phenomena. In this case, the center of attraction is not at the center of the sphere, but at some other point, and therefore the body moves in an ellipse. This is true of all bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. It is also true of those bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. 3. Elliptical motion of celestial phenomena. In this case, the center of attraction is not at the center of the sphere, but at some other point, and therefore the body moves in an ellipse. This is true of all bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. It is also true of those bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. 4. Elliptical motion of celestial phenomena. In this case, the center of attraction is not at the center of the sphere, but at some other point, and therefore the body moves in an ellipse. This is true of all bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. It is also true of those bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. 5. Elliptical motion of celestial phenomena. In this case, the center of attraction is not at the center of the sphere, but at some other point, and therefore the body moves in an ellipse. This is true of all bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. It is also true of those bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. 6. Elliptical motion of celestial phenomena. In this case, the center of attraction is not at the center of the sphere, but at some other point, and therefore the body moves in an ellipse. This is true of all bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. It is also true of those bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. 7. Elliptical motion of celestial phenomena. In this case, the center of attraction is not at the center of the sphere, but at some other point, and therefore the body moves in an ellipse. This is true of all bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. It is also true of those bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. 8. Elliptical motion of celestial phenomena. In this case, the center of attraction is not at the center of the sphere, but at some other point, and therefore the body moves in an ellipse. This is true of all bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. It is also true of those bodies that move in a circular orbit about any point whatever, such as the sun, or the earth itself. 9. Elliptical motion of celestial phenomena. In this case, the center of attraction is not at the center of 324 **ASTRONOMY.** An astronomy becomes less complicated, in the first place, when we consider that the earth is a spherical sphere. If the spectator be at the equator, the horizon will appear to be a circle, and the horizon, consequently, simply circular. But if he be at the poles, so that the horizon is perpendicular to his sight, he sees only two points, which are called the poles of the horizon. And as these circles are always placed at right angles to each other, they are called the meridians of the horizon. The observer is in this position at the equator all the heavenly bodies, whether they rise or set, appear to move on an equal time above and below the horizon, and have their greatest height at noon. The observer being at the pole, he sees nothing but the right angle of the horizon. Focal point. Fig. 22. At the pole, therefore, the equator will be represented in a circle, and the horizon in two points. In order to explain this proposition, let us suppose that we have a EQ with HR, so that the equator will coincide with the circle of latitude. Let us now draw a line from H to R, and another from H to Q. These lines will represent the horizon. Now, if we take any point on the circle above the horizon, and which changes its definition, we shall find that it is exactly opposite to one on the same altitude; and therefore it must be seen at the same altitude; and this is what actually happens. Because having a perfect circle for an equator, it is perfectly horizontal; and having two points for a horizon, it is perfectly vertical. Therefore, whatever body rises or sets on one side of the equator will be seen on the other side at the same time; and whatever body rises or sets on one side of the horizon will be seen on the other side at the same time. This is what actually happens; and it is evident by observing that about the 10th September of this year (1856), the sun rose at 7 o'clock in the morning at New York, and set at 7 o'clock in the evening at Buenos Ayres; and yet both places are nearly 1000 miles apart. On this principle, it is easy to understand why those who live near the poles see no stars at night; because there is no horizon for them to look over; and those who live near the equator see no stars during daylight hours; because there is no horizon for them to look over. Of the change of seasons. Fig. 23. As we have already said, those bodies which are not subject to a change of declination, and some of those which are subject to a very small change, are too insignificant to be attended to in this book. But those bodies which are subject to a considerable change of declination, in consequence of their proper motion round the earth, and also those which possess a great number of words in explaining these causes, put together make up a very considerable part of our knowledge of astronomy. It is evident that if we attempt to describe all these causes in detail, we shall not be able to do so without making this book too long; but I shall endeavour to give a general idea of them. Against the sun. Fig. 24. It is evident that if we attempt to describe a great deal of these causes in detail, we shall not be able to do so without making this book too long; but I shall endeavour to give a general idea of them. Against the moon. Fig. 25. Here lies one difficulty which has been frequently brought forward against our system of astronomy. It has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, the sun, moon and earth--then we cannot account for certain phenomena which occur every day. For instance, it has been said that if we suppose that there are three bodies revolving around us--namely, 325 **Astronomy** In astronomy he will be sometimes to the north of the equator; sometimes to the south of it; sometimes at right angles with it; sometimes parallel with it; and at other times in any other direction whatever. In short he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatever drawn through the center of our globe; or rather he will be somewhere between any two points whatever on any line whatsoever 326 **Astronomy** In astronomy he will be sometimes to the north of the equator; sometimes to the south of it; sometimes at right angles with it; sometimes parallel with it; and at other times in any other direction whatsoever. In short he will be somewhere between any two points whatsoever on any line whatsoever drawn through the center of our globe; or rather he will be somewhere between any two points whatsoever on any line whatsoever drawn through the center of our globe; or rather he will be somewhere between any two points whatsoever on any line whatsoever drawn through the center of our globe; or rather he will be somewhere between any two points whatsoever on any line whatsoever drawn through the center of our globe; or rather he will be somewhere between any two points whatsoever on any line whatsoever drawn through the center of our globe; or rather he will be somewhere between any two points whatsoever on any line whatsoever drawn through the center of our globe; or rather he will be somewhere between any two points whatsoever on any line whatsoever drawn through the center of our globe; or rather he will be somewhere between any two points whatsoever on any line whatsoever drawn through the center of our globe; or rather he will be somewhere between any two points whatsoever on any line whatsoever drawn through the center of our globe; or rather he will be somewhere between any two points whatsoever on any line whatsoever drawn through the center of our globe; or rather he will be somewhere between any two points whatsoever on any line whatsoever drawn through the center of our globe; or rather he will be somewhere between any two points whatsoever on 327 **Astronomy** In astronomy he will be sometimes to the north of the equator; sometimes to the south of it; sometimes at right angles with it; sometimes parallel with it; and at other times in任何其他方向。在短时间里，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的位置；或者更确切地说，他将处于任何两点之间的位置，无论这些点位于地球的中心线上的任何直线上的 328 **Astronomy** In astronomy he will be sometimes to the north of the equator; sometimes to the south of it; sometimes at right angles with it; sometimes parallel with it; and at other times in many other directions. In short time intervals within a few years' time, he may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing 329 **Astronomy** In astronomy he will be sometimes to the north of the equator; sometimes to the south of it; sometimes at right angles with it; sometimes parallel with it; and at other times in many other directions. In short time intervals within a few years' time, he may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing through his own position. He may move from one point to another point along a straight line passing 330 **Astronomy** In astronomy he will be sometimes to the north of the equator; sometimes to the south of it; sometimes at right angles with it; sometimes parallel with it; and at other times in many other directions. In short time intervals within a few years' time, he may move from one point to another point along a straight line passing 331 **Astronomy** In astronomy he will be sometimes to the north of the equator; sometimes to the south of it; sometimes at right angles with it; sometimes parallel with it; and at other times in many other directions. In short time intervals within a few years' time, he may move from one point to another point along a straight 332 **Astronomy** In astronomy he will be sometimes to the north of the equator; sometimes to the south of it; sometimes 333 **Astronomy** In astronomy he will be sometimes to the north 334 **Astronomy** In astronomy he will be sometimes 335 **Astronomy** In astronomy he will be sometime 336 **Astronomy** In astronomy he w 337 **Astronomy** In astronomy he w 338 **Astronomy** In astronomy he w 339 **Astronomy** In astronomy he w 340 **Astronomy** In astronomy he w 341 **Astronomy** In astronomy he w 342 **Astronomy** In astronomy he w 343 **Astronomy** In astronomy he w 344 **Astronomy** In astronomy he w 345 **Astronomy** In astronomy he w 346 **Astronomy** In astronomy he w 347 **Astronomy** In astronomy he w 348 **Astronomy** In astronomy he w 349 **Astronomy** In astronomy he w 350 **Astronomy** Since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since since ASTRONOMY. 525 place of noon, so that when it has attained its highest point, it will have been 12 hours since the sun's inferior, or south, of the equator in southern latitude; consequently, at this time, the sun will be situated in the ecliptic of either tropic, according to the sign of the zodiac in which they are, except those on the equator, who, as we have seen, have no sign. The sun will then be in the same place as it was at the beginning of the day. Beyond the tropics, either to such or such the sun is lower than at the equator. In this case, the sun being farther from the equator than the extreme de- gree of declination of the sun, it will be found that the two poles of the circle will have no part in their course. The sun will therefore be one and one only in each of these circles when the sun is at its highest point. This fact may be immediately obvious by referring to the preceding table. From these circles to the poles themselves the sun is not visible. But when it is below the horizon, in the actual poles, the night is still Table I. For the section of the heavens between 0° and 90°.
Green. Value of the Temperature. Case in which temperature requires an increase of heat.
I. Hypothecation. Angle opposite the green leg. If the sun be below these lines.
Its sin hypotenuse. If it be above these lines.
The given leg. If it be above these lines.
Its sin hypotenuse. If it be below these lines.
Dihedrals. If it be above these lines.
II. Hypothecation. Its sin hypotenuse. If it be above these lines.
The given leg. If it be below these lines.
Its sin hypotenuse. If it be above these lines.
Dihedrals. If it be below these lines.
III. Hypothecation. Its sin hypotenuse. If it be above these lines.
The given leg. If it be below these lines.
Its sin hypotenuse. If it be above these lines.
Dihedrals. If it be below these lines.
526 # ASTRONOMY. Astronomy. In working by logarithms the reader must observe, that when he has to find the value of any given quantity, 0 must be added to the index, and when it is required to find the value of any quantity less than the index, then between the two angles are given, logarithms of which are to be subtracted from the index. Thus when the two angles are given, logarithms of which are to be subtracted from the index, one angle may be $x$ and the other $y$, or one angle may be $x$ and the other $180 - x$ or one angle may be $x$ and log. cos $x$ may be $- y$ or log. $\cos y$ may be $- x$. Quadrilateral triangle. In a quadrilateral triangle of the quadrilateral side let called opposite to one of them, and let the angle that side be called hypotenuse, the other sides be called adjacent to each other, and let the sum of all the ratios of all the cases will be as the shown table takes the right or wrong form.
Given. Required. Values of the quantities required.
I. Side opposite to one of them. By common sense.
Tenth side. Let full a perp. = 1
Third side. Side containing a perp. = 1
Third angle. Let full a perp. = 1
II. Side opposite to one of them. By common sense.
Twelfth side and a side opposite to one of them. Let full a perp. = 1
Third side. Lateral a perp. = 1
III. An angle opposite to one of them. Lateral a perp. = 1
Twelfth side and included angle. Lateral a perp. = 1
Third side. Lateral a perp. = 1
IV. A side opposite to one of them. Lateral a perp. = 1
A side and the hypotenuse to gleve. Lateral a perp. = 1
Third angle. Lateral a perp. = 1
Napier's analogue for right angled spherical bi- sected triangles. Napier's circular part was, the complement of the angles that lie on either right angles, the complement of which is called Napier's sine, and is denoted by sin. A being right angle, the parts are no. 1, 2, 3, 4, C, and D, and the two parts next adjacent, so to either side as they are called (being called adjacent parts) and the other two opposite parts, thus: C + D = A + B = 90°. And if we take half of this circle, we have half of a middle part or rectangle of the tangents and sin of such middle part as rectangle of the cosines and sin of such middle part as rectangle of the cosines and sin of such middle part as rectangle of the cosines and sin of such middle part as rectangle of the cosines By making the transformations above explained, this table will give all kinds of spherical triangles. Time II. For the solution of adjoin cyclical spherical triangles.
) # ASTRONOMY.
Table II. - Continued.
Given. Required. Values of the quantities required.
Y. Let $a$, $b$, $c$ be the three sides; $A$, $B$, $C$ the angles; $\beta$ and $\gamma$ the included angles. $\sin \beta = \frac{a}{2R}$, $\sin \gamma = \frac{b}{2R}$, $\sin (A - B) = \frac{c}{2R}$, etc.
An angle by one side, its half. $\cos \alpha = \frac{a^2 + b^2 - c^2}{2ab}$
The three sides. $\cos \alpha = \frac{a^2 + b^2 - c^2}{2ab}$
VII. Let $a$ be the sum of the angles $A$, $B$, $C$, and $B$ and $C$ be adjacent to $a$, the sine expressed by $\sin (A - B)$ and $\sin (A - C)$. $\cos \alpha = \frac{a^2 + b^2 - c^2}{2ab}$
An angle by the sides of the triangle. $\cos \alpha = \frac{a^2 + b^2 - c^2}{2ab}$
The three angles. $\cos \alpha = \frac{a^2 + b^2 - c^2}{2ab}$
**TABLE III.** For the solution of all the cases of oblique spherical triangles, by the analogy of Napier.
Given. Required. Values of the numbers required.
I. Side opposite to the other given angle. By the common analogy: sin
Two angles and the included side, to one of them. The size of the angle not given is equal to the size of the opposite side.
Third side, Third angle. Out of its half $\sin \frac{\alpha}{2} = \frac{a}{2R}$, sin $\beta = \frac{b}{2R}$, sin $\gamma = \frac{c}{2R}$, etc., out of all these angles, sin $\beta - \gamma = \frac{b - c}{2R}$, etc., out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides, out of all these angles, out of all these sides,
II. Angle opposite to the other known angle. By the common analogy:
Two sides and opposite angle. $\cos x = \frac{a^2 + b^2 - c^2}{2ab}$
Third angle. $\cos x = \frac{a^2 + b^2 - c^2}{2ab}$
III. Third side. The two other angles and the included side. By common analogy:
Third side. The two other angles and the included side. $\cos x = \frac{a^2 + b^2 - c^2}{2ab}$
Third side. The two other angles and the included side. $\cos x = \frac{a^2 + b^2 - c^2}{2ab}$
IV. Third side. The two other angles and the included side.

VII. Either of the three angles...

**Astronomy** **4. Problems relative to the determination of the plane of the ecliptic.** **53. It is obvious from what we have stated relative to the latitude that the declination of the sun at any time is the same as the mean distance in latitude of the place of the observer, from which the sun is at the meridian, and that this place must be located on the plane of the ecliptic.** **Problem I.** To find the latitude of any place on the earth's surface. 1. To determine the latitude of any place on the earth's surface. 2. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 3. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 4. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 5. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 6. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 7. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 8. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 9. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 10. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 11. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 12. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 13. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 14. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 15. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 16. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 17. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 18. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 19. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 20. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 21. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 22. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 23. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 24. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 25. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 26. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 27. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 28. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 29. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 30. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 31. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 32. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 33. The latitude of any place on the sphere is measured by its distance from the equator and south pole. 34. The latitude of any place on A S T R O N O M Y. 529 **ADVERBATE** EXAM. 3. Let it be required to determine the time at which the sun will appear at the meridian on the 15th of February, 1810. The 15th day by sundial is 11 hours 47 minutes, and the sun's altitude is 2° 16' 47". Consequently, referring to the same figure, we shall find that the sun will rise at the meridian at 11 hours 47 minutes, and the sun's altitude will be 2° 16' 47". Q. What is the time when the sun will set? Ans. It will be found by referring to the same figure, that the sun will set at the meridian at 20 hours 30 minutes, and the sun's altitude will be 2° 16' 47". Q. How many degrees will the sun's altitude be at noon? Ans. It will be found by referring to the same figure, that the sun's altitude will be 2° 16' 47" at noon. Q. What is the time when the sun will be at its highest point? Ans. It will be found by referring to the same figure, that the sun will be at its highest point at 12 hours, and the sun's altitude will be 2° 16' 47". Q. What is the time when the sun will be at its lowest point? Ans. It will be found by referring to the same figure, that the sun will be at its lowest point at 6 hours, and the sun's altitude will be 2° 16' 47". Q. What is the time when the sun will be at its lowest point? Ans. It will be found by referring to the same figure, that the sun will be at its lowest point at 6 hours, and the sun's altitude will be 2° 16' 47". Q. What is the time when the sun will be at its lowest point? Ans. It will be found by referring to the same figure, that the sun will be at its lowest point at 6 hours, and the sun's altitude will be 2° 16' 47". Q. What is the time when the sun will be at its lowest point? Ans. It will be found by referring to the same figure, that the sun will be at its lowest point at 6 hours, and the sun's altitude will be 2° 16' 47". Q. What is the time when the sun will be at its lowest point? Ans. It will be found by referring to the same figure, that the sun will be at its lowest point at 6 hours, and the sun's altitude will be 2° 16' 47". Q. What is the time when the sun will be at its lowest point? Ans. It will be found by referring to the same figure, that the sun will be at its lowest point at 6 hours, and the sun's altitude will be 2° 16' 47". Q. What is the time when the sun will be at its lowest point? Ans. It will be found by referring to the same figure, that the sun will be at its lowest point at 6 hours, and the sun's altitude will be 2° 16' 47". Q. What is the time when the sun will be at its lowest point? Ans. It will be found by referring to the same figure, that the sun will be at its lowest point at 6 hours, and the sun's altitude will be 2° 16' 47". Q. What is the time when the sun will be at its lowest point? Ans. It will be found by referring to the same figure, that the sun will be at its lowest point at 6 hours, and the sun's altitude will be 2° 16' 47". Q. What is 530 # ASTRONOMY. Astronomy, say either heavenly body on the day of observation, or any other body which is observed to move in the heavens. The body, or the circle in which it is situated. There is a parallel line between the body and the observer's eye, and from this point, the perpendicular P.E., to p, from which the body appears to rise or set. The angle between the line of sight and the line of motion of the body, y, thus seen will be half the arc and apparent places of the body, x, and therefore the angle between the line of sight and the line of motion of the body, y, will be one half of the arc and apparent places of the body, x. This is because the body is on that circle, or the arc p on the equator, which will remain constant in time. Now think that m is being on some other circle than that of the equator, and that n is on another circle, and that r is on a right-angle triangle, right angled at n, and having mn as its base. By subtracting 180° from 180° + mn = 180° + mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = mn - 180° = nm # ASTRONOMY 531 Accordingly, the declination, $V$ to be imagined, and $x$ to be halved, we have three sides of the triangle $V_0P_0X$, viz., $V_0P_0 = 90^\circ - x$, $V_0X = x$, and $P_0X = 90^\circ + x$. The angle between these three sides, the angle required may be found by the sine rule (Table II), i.e., that $\sin Z = \frac{\sin V}{\sin P}$. Where the angle $Z$ is known, the angle $V$ may be determined, and conversely the angle $V$ is known, the angle $Z$ may be determined, and conversely the angle $Z$ is known. **Problem I.** Find the latitude of the place for the date and time given. Let us suppose that on a certain day at a certain hour, the sun will rise at a certain place with a certain altitude. We must find the latitude of this place. To do this, we first determine the declination of the sun at that time, which is done by means of a table of declinations. This table gives the declination of the sun for each day of the year. We then subtract this declination from 90 degrees to get the latitude of the place. For example, if the sun rises at 6 o'clock in the morning at a certain place with an altitude of 45 degrees, we can find from our table that the declination of the sun at that time is 45 degrees. We then subtract 45 degrees from 90 degrees to get 45 degrees as the latitude of the place. But as both the refraction and the equator are neglected in this problem, we must also take into account their effects. The refraction causes the sun to appear higher than its actual position, while the equator causes it to appear lower than its actual position. These effects must be taken into account when determining the latitude of a place. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude of a place is determined by measuring its distance north or south of the equator. This distance is measured in degrees, minutes, and seconds. The latitude of a place is usually expressed as a number between 0 and 90 degrees. The latitude 532 # ASTRONOMY. Anomaly will be the shortest possible when it is zero, because then the sine of the angle is equal to the cosine of the angle, and the equation will vanish. But this is only possible when the tangent $Z_0$ is reduced to the arc $Z_0$, that is, when the point falls within the interval between $Z_0$ and $Z_0 + \pi$. This is impossible, since $Z_0$ is the vertical line, lying within the small circle centered at $P$. Hence, we have $\sin Z_0 = 0$, which means that $Z_0 = 0$ or $\pi$. It is also manifest, that if $P$ increases, the opposite case occurs, namely, that $\sin Z_0 = 1$, which means that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. In these instances, the point will approach as near as possible to the circumference of the circle. In these instances, the point will approach as near as possible to the circumference of the circle. The limits of $Z_0$ are $Z_0 - \frac{\pi}{2}$ and $Z_0 + \frac{\pi}{2}$. Thus, the intercepted part of the arc will be less than $\frac{\pi}{2}$ and consequently may have the value $z = 0$ or $\pi$. But this is impossible, since we have already seen that the shortest twilight will always be at least half a day. Therefore, we must conclude that the arc $Z_0$ must be greater than $\frac{\pi}{2}$ and consequently must be less than $\pi$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\pi}{2}$. Therefore, we can say that $Z_0 > \frac{\pi}{2}$ and consequently must be less than $\pi$. We have shown that $\sin Z_0 = 1$, so we can conclude that $Z_0 = \frac{\pi}{2}$ or $\frac{3\π ASTRONOMY. 533 Astronomy. where P = 187° 5' 28" (or 1° 2' 50" according to the N. A. M.) half sun = 180° - 187° 5' 28" = 2° 5' 32" half dif. = 360° - 187° 5' 28" = 172° 44' 32" The former in time answers to 2° 5' 32", the latter to the time of the beginning of the day. The former showing the time when the evening twilights begin, and the latter that of the morning twilight. The above numbers, taken respectively from II., will be found sufficient for all practical purposes. Difficulties between the two times of the sun's rising and setting at different latitudes, and even at different times of the year, are so great, that we have no means of determining with any degree of accuracy their exact value. The only method which can be adopted is to observe the times of the sun's rising and setting at different places, and then to calculate the difference between them by means of a table of latitudes. This method is very tedious, and requires a great deal of care and attention on the part of the observer. It is also subject to many errors, and cannot be relied upon with much confidence. IV. Description and use of the most important astronomical instruments. The following is a brief description of some of the most important astronomical instruments, together with a short account of their uses. 1. Telescope. The telescope is one of the most useful instruments in astronomy. It is used for observing distant objects, such as stars, nebulae, and other celestial bodies. It consists of a lens or a series of lenses, which are arranged in such a way that they form an image of the object being observed. The image is then magnified by a system of mirrors or lenses, which are placed behind the objective lens. The telescope is usually mounted on a tripod, which allows it to be pointed in any direction desired. 2. Quadrant. The quadrant is another instrument used in astronomy. It is similar to the telescope, but instead of forming an image of the object being observed, it measures the angle between two lines drawn from the center of the quadrant to two points on the horizon. This angle is called the altitude of the object being observed. 3. Sextant. The sextant is a small instrument used in navigation. It is similar to the quadrant, but instead of measuring angles, it measures distances. It is used for measuring the distance between two points on the horizon. 4. Compass. The compass is an instrument used in navigation. It is similar to the sextant, but instead of measuring distances, it measures directions. It is used for determining the direction in which a ship is traveling. 5. Chronometer. The chronometer is an instrument used in navigation. It is similar to the sextant and compass, but instead of measuring distances and directions, it measures time. It is used for determining the time at which a ship is traveling. 6. Barometer. The barometer is an instrument used in meteorology. It is similar to the chronometer, but instead of measuring time, it measures pressure. It is used for determining the pressure at which a ship is traveling. 7. Thermometer. The thermometer is an instrument used in meteorology. It is similar to the barometer, but instead of measuring pressure, it measures temperature. It is used for determining the temperature at which a ship is traveling. 8. Hygrometer. The hygrometer is an instrument used in meteorology. It is similar to the thermometer, but instead of measuring temperature, it measures humidity. It is used for determining the humidity at which a ship is traveling. 9. Anemometer. The anemometer is an instrument used in meteorology. It is similar to the hygrometer, but instead of measuring humidity, it measures wind speed and direction. It is used for determining the wind speed and direction at which a ship is traveling. 10. Barograph. The barograph is an instrument used in meteorology. It is similar to the anemometer, but instead of measuring wind speed and direction, it measures pressure changes over time. It is used for determining how pressure changes affect weather patterns. 11. Barograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thermograph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-thergraph-hergraph-hergraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregraph-heregr 9/22 VIII. Vol. III. the quality that must not be neglected in any complete description of astronomy; therefore a tendency to increase the apparent value discovered by this science would be admirable; but it seems impossible to extend its limits; for though its spectacle may be grand, yet its effect on our senses does not exceed what it has been hitherto known; hence its value must be limited; and this limit is not likely to be increased until some new discovery shall be made, which shall show us that we have not yet exhausted all that nature has now to offer us; nor shall we ever attain our purpose to explain the instruments and methods employed by astronomers; for these are merely tools for aiding their purposes, and the nature and quantity of the light they receive from nature are not sufficient thus checked, as we see them proper for their end. IV. Description and use of some of the most important astronomical instruments. The following are descriptions and uses of some of the most important astronomical instruments: 1) Telescope: A telescope is an optical device that magnifies distant objects by focusing light through a lens or a series of lenses onto a screen or photographic film. 2) Quadrant: A quadrant is an instrument used in astronomy that measures angles between two lines drawn from a point on Earth's surface to two points on Earth's horizon. 3) Sextant: A sextant is a small instrument used in navigation that measures distances between two points on Earth's horizon. 4) Compass: A compass is an instrument used in navigation that measures directions. 5) Chronometer: A chronometer is an instrument used in navigation that measures time. 6) Barometer: A barometer is an instrument used in meteorology that measures pressure. 7) Thermometer: A thermometer is an instrument used in meteorology that measures temperature. 8) Hygrometer: A hygrometer is an instrument used in meteorology that measures humidity. 9) Anemometer: An anemometer is an instrument used in meteorology that measures wind speed and direction. 10) Barograph: A barograph is an instrument used in meteorology that measures pressure changes over time. 11) Barograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermograph-Thermographic-Thergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Tergraphic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Terographic-Tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterraphic-tterpheric-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical-thetrical9/22 534 ASTRONOMY. A commentary on the book of Job. The first chapter of the book of Job is a dialogue between Job and his friends, in which he complains of the calamities that have befallen him, and asks them to explain the causes of these misfortunes. The second chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The third chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The fourth chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The fifth chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The sixth chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The seventh chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The eighth chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The ninth chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The tenth chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The eleventh chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The twelfth chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The thirteenth chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The fourteenth chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The fifteenth chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The sixteenth chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The seventeenth chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The eighteenth chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The nineteenth chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The twentieth chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The twenty-first chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The twenty-second chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The twenty-third chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The twenty-fourth chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The twenty-fifth chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The twenty-sixth chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The twenty-seventh chapter is a reply by Job, in which he denies the explanations given by his friends, and asserts that he has no fault to blame for the calamities that have befallen him. The twenty-eighth chapter is a reply by Job's friends, in which they attempt to explain the causes of the calamities that have befallen Job, and to show that they are not due to any fault of Job's own. The twenty-ninth chapter is a reply byJob ASTRONOMY. 535 Astronomy: the same time since we are constructed so as to answer the question, "What is the distance between the earth and the sun?" we must confine our attention to only one of the most perfect of such, but, on the contrary, we must examine all of them with equal care, at length, and endeavour to illustrate the advantages and defects of each. Of astronomical peculiarities. 1. There is no place in the heavens where the former case (as they are constantly met with in a tripod, and not in a quadrant) can be observed. The reason of this is, that the quadrant is not made to follow the body observed in its apparent motion, but is fixed in a perpendicular position, and therefore cannot be turned round to observe any other body than that which is in the plane of the revolution against a substantial line, and in the same direction. 2. Portable telescopic quadrant. The great variety of forms under which this instrument may be found is owing to the different opinions entertained by different authors for adapting it to its various uses. In some cases it is made very large, in others very small; in some cases it is made for use with a telescope, in others without it; and in some cases it is made for use with a quadrant, in others without it. But whatever may be its form, and however much it may differ from the ordinary quadrant, yet it will always be found to consist of two parts, viz. 1st. A vertical axis, which turns about a point at the top of the quadrant; 2ndly. A horizontal axis, which turns about a point at the bottom of the quadrant. These two axes are called respectively the upper and lower axes. Now, when these two axes are turned round together, they will turn either up or down; but when they are turned separately, they will turn either left or right. Hence it follows that when these two axes are turned together, they will describe a circle; but when they are turned separately, they will describe two circles. And hence it appears that when these two axes are turned together, they will describe a circle; but when they are turned separately, they will describe two circles. And hence it appears that when these two axes are turned together, they will describe a circle; but when they are turned separately, they will describe two circles. Fig. 23. Fig. 23 represents a portable quadrant, constructed by Mr. John Gough, Esq., of London. Gough's quadrant. The tripod on which it is mounted has three legs; and the head of the tripod is provided with three arms or legs, which are adjustable by screws. The upper arm is provided with a horizontal plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The lower arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The middle arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The upper arm is provided with a horizontal plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The lower arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The middle arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The upper arm is provided with a horizontal plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The lower arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The middle arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The upper arm is provided with a horizontal plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The lower arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The middle arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The upper arm is provided with a horizontal plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The lower arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The middle arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The upper arm is provided with a horizontal plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The lower arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The middle arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The upper arm is provided with a horizontal plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The lower arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The middle arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The upper arm is provided with a horizontal plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The lower arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The middle arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The upper arm is provided with a horizontal plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The lower arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The middle arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The upper arm is provided with a horizontal plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The lower arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The middle arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The upper arm is provided with a horizontal plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The lower arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The middle arm is provided with a vertical plate or base upon which rests the quadrant; and this base is 536 provided with three feet or legs, which are adjustable by screws. The upper arm is provided with a horizontal plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The lower arm is provided with a vertical plate or base upon which rests the quadrant; and this base is provided with three feet or legs, which are adjustable by screws. The 537 middle 538 arm 539 is 540 provided 541 with 542 a 543 vertical 544 plate 545 or 546 base, 547 upon 548 which 549 rests 550 the 551 quadrant; 552 and 553 this 554 base 555 is 556 provided 557 with 558536 A S T R O N O M Y. Astronomy, if there be any at the same time, which is to be observed by the telescope, must be adjusted so as to align with the vertical line, and then to adjust by the vertical line, for the sake of the quadrant, and that the quadrant may be placed exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and measure its altitude exactly on the meridian, and observe by day; but if there be any at night by night; when this distance is made known by means of a glass of telescope should not be disturbed. The telescope should be placed in such a manner that it may be seen through without being obscured by any other object. It is taken for granted that all observations will be made during daylight hours. During these times it is necessary to make use of a quadrant or sextant. The quadrant or sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The quadrant is used for measuring angles. The sextant is used for measuring angles. The telescope should be placed in such a manner that it may be seen through without being obscured by any other object. It takes place during daylight hours. During these times it is necessary to make use of a quadrant or sextant. The quadrant or sextant measures angle. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants are usually made of wood. The quadrants areusuallymadeofwood. Page 108 Phase Anomaly by day, and by night by night. When this distance has been determined by means of a glass telescope should not be disturbed, the telescope should be placed in such a manner that it may be seen through without being obscured by any other object. It takes place during daylight hours. During these times it is necessary to make use of a quadrant or sextant. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or sextans measures angle. Quadrats or Sextan is a device that can be adjusted to show how much time has passed since a certain event occurred in history (such as a person's birthday). It works by counting down from a specific date until it reaches zero again after one full cycle has passed (e.g., 365 days). There have been many different types of calendars throughout history: - Roman calendar - Gregorian calendar - Julian calendar - Hebrew calendar - Islamic calendar - Buddhist calendar - Hindu calendar - Chinese calendar - Japanese calendar - Korean calendar - Vietnamese calendar - Thai calendar - Lao calendar - Cambodian calendar - Burmese calendar - Thai lunar calendar - Lao lunar calendar - Cambodian lunar calendar - Burmese lunar calendar - Thai solar calendar - Lao solar calendar - Cambodian solar calendar - Burmese solar calendar - Thai lunisolar calendar - Lao lunisolar calendar - Cambodian lunisolar calendar - Burmese lunisolar calendar There have been many different types of calendars throughout history: - Roman calendar - Gregorian calendar - Julian calendar - Hebrew calendar - Islamic calendar - Buddhist calendar - Hindu calendar - Chinese calendar - Japanese calendar - Korean calendar - Vietnamese calendar - Thai calendar - Lao calendar - Cambodian calendar - Burmese calendar - Thai lunar calendar - Lao lunar calendar - Cambodian lunar calendar - Burmese lunar calendar - Thai solar calendar - Lao solar calendar - Cambodian solar calendar - Burmese solar calendar There have been many different types of calendars throughout history: Roman Calendar Gregorian Calendar Julian Calendar Hebrew Calendar Islamic Calendar Buddhist Calendar Hindu Calendar Chinese Calendar Japanese Calendar Korean Calendar Vietnamese Calendar Thai Calendar Lao Calendar Cambodian Calendar Burmese Calendar Thai Lunar Calendar Lao Lunar Calendar Cambodian Lunar Calendar Burmese Lunar Calendar Thai Solar Calendar Lao Solar Calendar Cambodian Solar Calendar Burmese Solar Calendar Thai Lunisolar Calendar Lao Lunisolar Calendar Cambodian Lunisolar Calendar Burmese Lunisolar Calendar ASTRONOMY. 537 Astronomy may be used in my place to ascertain the rate of a comet, or any other body which moves in a circle about the meridian, for determining also the right ascension of the sun at any given time, and the declination of any star, only that we must describe no place in this place. The instrument I have described is called a quadrant, and is represented in fig. 34. It consists of two pieces of wood, one of which is called the arm, and the other the quadrant. The arm is divided into degrees, and each degree is marked with a line, so that by turning the quadrant round, one can find out how many degrees there are between any two points on the horizon. This instrument is used in the quadrant, and is called the quadrant. The arm is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant is made of wood, and is about 30 inches in length. The quadrant Phase Astronomy may be used to determine the rate at which a comet moves around the meridian; for determining also the right ascension (or hour angle) at any given time; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east or west a star lies from the meridian; or to find out how far north or south a star lies from the meridian; or to find out how far east Phase Astronomy eastern part of this tractment it has been employed ; two which are occupied by trees ; one which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass ; another Phase Astronomy which has been planted with grass : after whiich thw are te brought into some common use To effect this, A diagram showing an astronomical instrument. When the level hangs up on its staff fasten it first by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means of screws at both ends so that it will not fall down when it comes into contact either side by means 538 ASTRONOMY. Atmosony. seems telescopes have the eye-glass and cell, which are fixed, others have the lens fixed, and the two glasses move about on the axis of the telescope. In drawing out the eye-piece, adjust the telescope so that the object appears to be at infinity, then by moving the focus, it will move the nearer one, or other former, from the eye-piece. When the object is very distant, it appears perfectly distinct, and the telescope will be aligned with it. When it is near, it will appear blurred, push in, or draw out, the eye-piece, till the vision will be perfect. The telescope may be used to measure the sun's parallax, or its distance, and a planet, apart from perfectly distinct and clear. As it is of importance to see the telescope adjusted properly before taking any observations, I shall here give some directions for doing this. Try whether it is so or not, by means of a small mirror placed in front of the eye-piece. If it does not reflect back a bright image of the object under observation, it is not properly adjusted. If it does reflect back a bright image of the object under observation, it is not properly adjusted. To bring a transit instrument into the plane of the meridian. Take the altitude of one star, noting the time when the watch or clock, and likewise find the apparent time, when the altitude of another star is observed. The difference between these times and seconds is called the time of transit. If both stars are observed at once and found to be in the same place in the heavens at different times, they are said to be in transit. This is only true when they are seen at their greatest declination. If they are seen at their greatest declination, they are said to be in transit. This is only true when they are seen at their greatest declination. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across the meridian. The time of transit is determined by observing the altitude of one star at different times during its passage across 14 or 9/22. Astronomy may be convenient, or as it can be seen distinctly marked better every astronome. See the first vol. of the Transactions of the Royal Society of Edinburgh, p. 305. At the preceding article we have supposed that the earth's axis is inclined to the plane of its orbit, but this from the time which may be inferred, you shall see proper means of determining whether this inclination has been altered by any change in the body of the earth, or by any other cause. The method of adjusting the clock with respect to the inclination of the earth's axis will be described hereafter. Exposition of the subject. The meridian, being the centre of the field of the celestial sphere, is always in the same place at all times, and every one who has observed the stars knows that they appear to move in a circle round it. This fact is also true of the moon, and it is evident that when the moon is in opposition to the sun, she will always be in the same place at all times. It is therefore evident that if we could find out how long it takes for the moon to make one circuit round the earth, we should know exactly what time it is at any given moment. This is called the sidereal period of the moon, and it is equal to 27 days, 7 hours, 43 minutes, and 12 seconds. Now let us suppose that we have a clock which runs uniformly, and that we set it so that it shows the time when the moon passes over a certain point on her orbit. We then wait until she has made one complete circuit round the earth, and then we note down what time it is at that moment. We shall find that it is exactly two weeks after she passed over that point. This is because she makes one circuit round the earth in 27 days, 7 hours, 43 minutes, and 12 seconds, and since there are 1440 minutes in a day, we must multiply this number by 1440 to get the total number of minutes in two weeks. This gives us 438600 minutes, which is equal to 731 days, 1 hour, and 20 minutes. Therefore we can say that if we set our clock so that it shows the time when the moon passes over a certain point on her orbit, and then wait until she has made one complete circuit round the earth, we shall find that it is exactly two weeks after she passed over that point. This method of determining the sidereal period of the moon was first proposed by Sir Isaac Newton in his "Principia Mathematica," and he gave a very accurate calculation of it. He found that the sidereal period of the moon was 27 days, 7 hours, 43 minutes, and 12 seconds, which agrees very closely with our modern observations. It is evident that if we could determine accurately the sidereal period of any other body in our solar system, we could use it as a standard for measuring time. For example, if we knew that Jupiter's sidereal period was 12 years, 8 months, and 20 days, we could use this as a standard for measuring time. This would give us a much more accurate measure of time than our present system based on the rotation of the earth. In conclusion I wish to say that I believe that this method of determining time by observing the motion of bodies in space is a very important one. It has been used successfully for many years and has led to many important discoveries. I hope that it will continue to be used in future investigations. 539 **Astronomy** The meridian being always in the same place at all times, and every one who has observed the stars knows that they appear to move in a circle round it. This fact is also true of the moon, and it is evident that when the moon is in opposition to the sun, she will always be in the same place at all times. It is therefore evident that if we could find out how long it takes for the moon to make one circuit round the earth, we should know exactly what time it is at any given moment. This is called the sidereal period of the moon, and it is equal to 27 days, 7 hours, 43 minutes, and 12 seconds. Now let us suppose that we have a clock which runs uniformly, and that we set it so that it shows the time when the moon passes over a certain point on her orbit. We then wait until she has made one complete circuit round the earth, and then we note down what time it is at that moment. We shall find that it is exactly two weeks after she passed over that point. This method of determining the sidereal period of the moon was first proposed by Sir Isaac Newton in his "Principia Mathematica," and he gave a very accurate calculation of it. He found that the sidereal period of the moon was 27 days, 7 hours, 43 minutes, and 12 seconds, which agrees very closely with our modern observations. It is evident that if we could determine accurately the sidereal period of any other body in our solar system, we could use it as a standard for measuring time. For example, if we knew that Jupiter's sidereal period was 12 years, 8 months, and 20 days, we could use this as a standard for measuring time. This would give us a much more accurate measure of time than our present system based on the rotation of the earth. In conclusion I wish to say that I believe that this method of determining time by observing the motion of bodies in space is a very important one. It has been used successfully for many years and has led to many important discoveries. I hope that it will continue to be used in future investigations. 539 **Astronomy.** According to observations to actual astronomical determinations. **1. Of solar and moon solar days, proper.** 906. We have seen that the earth performs its revolution around the sun once in a year, and that the interval between the return of any fund of the same name on the same day is one solar day; observing that by the same motion is here to be understood the motion of the sun about the earth, and not the motion of the earth about the sun. In the course of 365.4 hours, once in their inferior and once in their superior orbs, we have two names of solar days, which explain what is to be understood by a solar day, that is, the time taken by the sun to return to the same meridian altitude. This interval, then, is the time taken by the sun to return to the same meridian altitude. This interval, then, is the time taken by the sun to return to the same meridian altitude. This interval, then, is the time taken by the sun to return to the same meridian altitude. This interval, then, is the time taken by the sun to return to the same meridian altitude. **2. Of lunar and moon lunar days, proper.** 907. It will be seen in the following articles, that due to this reason, when we speak of a lunar day or part of a lunar day to return again in the same name, it will be understood that it is one lunar day or part of a lunar day to return again in the same name, it will be understood that it is one lunar day or part of a lunar day to return again in the same name, it will be understood that it is one lunar day or part of a lunar day to return again in the same name, it will be understood that it is one lunar day or part of a lunar day to return again in the same name. 908. The time from the passage of the moon over the meridian at its first appearance until its second passage over the same meridian was found equal to 24 hours; but since this was only an average right assumption, connected with this star, which had been observed during many years; therefore it was found necessary to make some experiments with this star, so as to ascertain whether this assumption was true or false; and these experiments were repeated on the second year, three times on each occasion; and it was found that this time was 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes. 909. The time from the passage of the moon over the meridian at its first appearance until its second passage over the same meridian was found equal to 24 hours; but since this was only an average right assumption, connected with this star, which had been observed during many years; therefore it was found necessary to make some experiments with this star, so as to ascertain whether this assumption was true or false; and these experiments were repeated on the second year, three times on each occasion; and it was found that this time was 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes. 910. The time from the passage of the moon over the meridian at its first appearance until its second passage over the same meridian was found equal to 24 hours; but since this was only an average right assumption, connected with this star, which had been observed during many years; therefore it was found necessary to make some experiments with this star, so as to ascertain whether this assumption was true or false; and these experiments were repeated on the second year, three times on each occasion; and it was found that this time was 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes. 911. The time from the passage of the moon over the meridian at its first appearance until its second passage over the same meridian was found equal to 24 hours; but since this was only an average right assumption, connected with this star, which had been observed during many years; therefore it was found necessary to make some experiments with this star, so as to ascertain whether this assumption was true or false; and these experiments were repeated on the second year, three times on each occasion; and it was found that this time was 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes. 912. The time from the passage of the moon over the meridian at its first appearance until its second passage over the same meridian was found equal to 24 hours; but since this was only an average right assumption, connected with this star, which had been observed during many years; therefore it was found necessary to make some experiments with this star, so as to ascertain whether this assumption was true or false; and these experiments were repeated on the second year, three times on each occasion; and it was found that this time was 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes. 913. The time from the passage of the moon over the meridian at its first appearance until its second passage over the same meridian was found equal to 24 hours; but since this was only an average right assumption, connected with this star, which had been observed during many years; therefore it was found necessary to make some experiments with this star, so as to ascertain whether this assumption was true or false; and these experiments were repeated on the second year, three times on each occasion; and it was found that this time was 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes. 914. The time from the passage of the moon over the meridian at its first appearance until its second passage over the same meridian was found equal to 24 hours; but since this was only an average right assumption, connected with this star, which had been observed during many years; therefore it was found necessary to make some experiments with this star, so as to ascertain whether this assumption was true or false; and these experiments were repeated on the second year, three times on each occasion; and it was found that this time was 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes; and therefore this time was found equal to 24 hours and 14 minutes. 915. The time from the passage of the moon over A S T R O N O M Y **541** **Observation.** It is obvious, that at some intermediate time between the two observations, the sun will have passed through some altitude or declination as in the first instance. Now, if we suppose that the sun has passed through some point of altitude or declination as in the second observation, the dis- tance between these two points will be equal to the time between the hours, or also the difference between the altitudes as observed by the two observers, multiplied by 360° divided by the number of degrees in a day, which gives us the hour, then, assuming the declination to be unknown, we can find it thus: $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\circ}$$ or $$D = \frac{360}{24} \times 30^{\circ} = 45^{\degree}\texttt{}$ **Procedure.** The method of determining the equinoctial point is very simple. We have observations of the kind from the time of one equinox to another. We know that at this time the sun will pass through some point of altitude or declination. We must determine what this point is. To do this we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrature or not. If it shall be necessary to use a mean of quadrature, we must ascertain whether it shall be necessary to use a mean of quadrant 542 **ASTRONOMY.** **Astronomy.** Waltham, in 1706. Copenhagen, in 1708. Cambridge, in 1709. Cambridge, in 1710. Cambridge, in 1713. Cambridge, in 1714. Cambridge, in 1715. Cambridge, in 1716. Cambridge, in 1717. Cambridge, in 1718. Cambridge, in 1719. Cambridge, in 1720. Cambridge, in 1721. Cambridge, in 1722. Cambridge, in 1723. Cambridge, in 1724. Cambridge, in 1725. Cambridge, in 1726. Cambridge, in 1727. Cambridge, in 1728. Cambridge, in 1729. Cambridge, in 1730. Cambridge, in 1731. Cambridge, in 1732. Cambridge, in 1733. Cambridge, in 1734. Cambridge, in 1735. Cambridge, in 1736. Cambridge, in 1737. Cambridge, in 1738. Cambridge, in 1739. Cambridge, in 1740. Cambridge, in 1741. Cambridge, in 1742. Cambridge, in 1743. Cambridge, in 1744. Cambridge, in 1745. Cambridge, in 1746. Cambridge, in 1747. Cambridge, in 1748. Cambridge, in 1749. Cambridge, in 1750. Cambridge, in 1751. Cambridge, in 1752. Cambridge, in 1753. Cambridge, in 1754. Cambridge, in 1755. Cambridge, in 1756. Cambridge, in 1757. Cambridge, in 1758. Cambridge, in 1759. Cambridge, in 1760. Cambridge, in 1761. Cambridge, in 1762. Cambridge, in 1763. Cambridge, in 1764. Cambridge, in 1765. Cambridge, in 1766. Cambridge, in 1767. Cambridge, in 1768. Cambridge, in 1769. The observations of Albericoz at Ancona show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is less than that of Jupiter's. The observations of the same astronomer at Lisbon show that the sun's diameter is greater than that of Jupiter's. The observations of the same astronomer at Lisbon show Fig. No. Observed by Mr. Waltham In his time of this comet is not known whether it was observed by Mr. Waltham or not. The circumstances are such as to render it necessary to examine this subject with great care and attention; and I have been led to do so by several considerations which I shall now proceed to state. Firstly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Secondly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Thirdly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Fourthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Fifthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Sixthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Seventhly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Eighthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Ninthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Tenthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Eleventhly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Twelfthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Thirteenthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Fourteenthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Fifteenthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Sixteenthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Seventeenthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Eighteenthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Nineteenthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Twentiethly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Twenty-firstly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Twenty-secondly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Twenty-thirdly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Twenty-fourthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Twenty-fifthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Twenty-sixthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Twenty-seventhly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Twenty-eighthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Twenty-ninethly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Thirty-ethyly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Thirty-firstly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Thirty-secondly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Thirty-thirdly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Thirty-fourthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Thirty-fifthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Thirty-sixthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Thirty-seventhly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Thirty-eighthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Thirty-ninthly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who have made very accurate measurements on this subject; and they have all found it to be true. Fortiethyly - It has been observed by several astronomers (amongst whom Messrs Bradley and Flamsteed) who Fig. observed by Mr Waltham in his time of this comet is not known whether he was here when he saw or not ASTRONOMY. 543 Anomaly. P = Q. Corollary, for instance, the two reflections are to be made at the same time. P + Q at $90^\circ$ (q - q') = 0. Therefore, since the sum of the two reflexions $p + q$ is given, the difference between them must be equal to zero, consequently, the sum of the two reflexions $p + q'$ is also given, but, by referring to the table extant on this sub-ject, we find that the sum of the two reflexions is equal to 90 degrees, and hence the two equations give $$p' = p - 90^\circ \quad q' = q + 90^\circ$$ Now, according to the law of refraction, he found $$\tan p' = \frac{1}{\tan Q}$$ $$\tan q' = \frac{\tan Q}{1}$$ wherein $p$ is $90^\circ$ and $q$ is $90^\circ$, and therefore, in order to ob-serve a correct result, the refracted ray must be parallel to the incident ray, which should be in one another the tangents of the ob- scured angles must be equal. Hence, $$p' = (q' - q) \cdot \frac{\tan Q}{1}$$ $$q' = (p' - p) \cdot \frac{\tan Q}{1}$$ or $$\tan p' = \frac{\tan Q}{\tan Q}$$ $$\tan q' = \frac{\tan Q}{\tan Q}$$ and by means of the new operator, he found $$\tan p' = \frac{\tan Q}{\tan Q}$$ $$\tan q' = \frac{\tan Q}{\tan Q}$$ But this result was not obtained, because the reflection is very near to the tangent of the second angle of incidence. For example, when a ray is reflected from a plane surface, may be illuminated as follows: Fig. 26. The angle of incidence is $\alpha$, and the angle of reflection is $\beta$. The angle of incidence is $\gamma$, and the angle of reflection is $\delta$. The angle of incidence is $\epsilon$, and the angle of reflection is $\zeta$. The angle of incidence is $\theta$, and the angle of reflection is $\phi$. The angle of incidence is $\psi$, and the angle of reflection is $\omega$. The angle of incidence is $\chi$, and the angle of reflection is $\eta$. The angle of incidence is $\xi$, and the angle of reflection is $\mu$. The angle of incidence is $\nu$, and the angle of reflection is $\tau$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the angle of reflection is $\pi$. The angle of incidence is $\tau$, and the angle of reflection is $\rho$. The angle of incidence is $\sigma$, and the 1 once or greater zenith distance, he employed the fine 2 of a telescope, which was sufficient to show that it was impossible for any star to be at a greater zenith distance than its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameter. This was shown by observing that when a star was seen at a distance less than its least visible diameter, it could not be seen again until it had passed beyond its least visible diameters. 3 This formula will serve to apply with considera- tion to all cases where there are no other factors involved. For instance: In case A has altitude 80° for 180°; B has altitude 70° for 180°; C has altitude 60° for 180°; D has altitude 50° for 180°; E has altitude 40° for 180°; F has altitude 30° for 180°; G has altitude 20° for 180°; H has altitude 10° for 180°; I has altitude 5° for 180°; J has altitude 2° for 180°; K has altitude 1° for 180°; L has altitude 0° for 180°; M has altitude -5° for 180°; N has altitude -10° for 180°; O has altitude -20° for 180°; P has altitude -30° for 180°; Q has altitude -40° for 180°; R has altitude -50° for 180°; S has altitude -60° for 180°; T has altitude -70° for 180°; U has altitude -80° for 180°. In this case we have: A = B + C + D + E + F + G + H + I + J + K + L + M + N + O + P + Q Therefore: A = B + C + D + E + F + G + H + I + J + K + L + M + N + O + P + Q # ASTRONOMY. Astronomy for every minute below 7.0000, or for every minute above 7.0000, is given by the table of refractions, with the repetition of tables of meridional parallaxes, and the product added or subtracted thereto, so as to make the sum of the figures in place or minus.
Ref. Dist. Reflex. Zen. Dist. Reflex. Zen. Dist. Reflex. Zen. Dist. Reflex.
0.00 0.00 25.5 44.9 63.8 87.3 114.7 143.7
0.01 0.01 25.5 44.9 63.8 87.3 114.7 143.7
0.02 0.02 25.5 44.9 63.8 87.3 114.7 143.7
0.03 0.03 25.5 44.9 63.8 87.3 114.7 143.7
0.04 0.04 25.5 44.9 63.8 87.3 114.7 143.7
0.05 0.05 25.5 44.9 63.8 87.3 114.7 143.7
0.06 0.06 25.5 44.9 63.8 87.3 114.7 143.7
0.07 0.07 25.5 44.9 63.8 87.3 114.7 143.7
0.08 0.08 25.5 44.9 63.8 87.3 114.7 143.7
0.09 0.09 25.5 44.9 63.8 87.3 114.7 143.7
Table of mean refractions, computed from the preceding formulae.
Zen.Dist.Reflex.Zen.Dist.Reflex.Zen.Dist.Reflex.
-2°-2°'-2°-2°'-2°-2°'-2°-2°'-2°-2°'-2°-2°'-2°-2°'-2°-2°'-2°-2°'
-1°-1°'-1°-1°'-1°-1°'-1°-1°'-1°-1°'-1°-1°'-1°-1°'-1°-1°'-1°-1°'
-6°-6°'-6°-6°'-6°-6°'-6°-6°'-6°-6°'-6°-6°'-6°-6°'-6°-6°'-6°-6°'
-5°-5°'-5°-5°'-5°-5°'-5°-5°'-5°-5°'-5°-5°'-5°-5°'-5°-5°'-5°-5°'
-4°-4°'-4°-4°'-4°-4°'-4°-4°'-4°-4°'-4°-4°'-4°-4°'-4°-4°'-4°-4°'
Zen.Dist.Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
Zen.Dist.
A S T R O N O M Y. 545 Correction to preceding table of refraction.
BAROMETER. FARRELL'S THERMOMETER. Please
Inches. Centes. Baros. Comets. Degres. Wahns. Wahns. Decres. Wahns. Wahns.
00 0000 276 280 0014 0023 0033 0043 0053 0063
02 0121 49 0007 245 0023 0043 0063 0083 0103
14 0141 79 0012 355 0043 0063 0083 0103 0123
66 0261 169 0025 555 0114 0143 0173 0213 0253
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Sr981a
Sr997o
Sr9981a
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Sr99981a
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Sr999981a
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Sr999999981a
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Inches:
Centes:
Baros:
Comets:
Degres:
Wahns:
Wahns:
Decres:
Wahns:
Wahns:
Decres:
Wahns:
Wahns:
Decres:
Wahns:
Wahns:
Decres:
Wahns:
Wahns:
Decres:
Wahns:
Wahns:
Decres:
Wahns:
Wahns:
Decres:
Wahns:
Wahns:
Decres:
Wahns:
Wahns:
546 Astronomy. 113. What we have hitherto stated relates chiefly to corrections requisite to be made in order to ascertain the true distance of the sun from the earth and the true time of its passage through the meridian. Such refinements will also explain some other interesting phenomena which will appear in the course of this evening twilight, the real appearance of the sun at the meridian, and the duration of its transit. Case of the vertical. 115. With respect to the twilight it arises when the sun is below the horizon and before it has passed through the meridian. It is therefore a phenomenon which is connected with the lower boundary of the atmosphere. In it, however that which is reflected by the body of the sun is not only seen by those who are beyond the horizon in evening but also by those who are before horizon in evening then it is seen by all those who are between them and even by those in winter as well as in summer. Now in former case heat felt more strongly than in winter In latter case on contrary felt less strongly than in summer therefore according to reflection of light it appears that there is greater heat in summer than in winter whereas according to reflection of light it appears that there is greater heat in winter than in summer thus in morning and longer in summer than in winter Consequently it is necessary that twilight begin when it still dark enough to feel a little heat and that investigations relative to time of absolute twilight shall be made with view to ascertain what number of degrees and how much they may therefore be supplied by artificial means. 116 Another effect of refraction as we have already seen (p. 480) is that it produces an apparent increase in consequence of refraction of sun's rays of its angular diameter This effect is very great when vertical diameter is diminished For assuming sun's diameter is 360° and that its apparent diameter is 35° 47 but that its actual diameter is 360° then its apparent diameter would be 35° 47 × 360 ÷ 360 = 35° 47 The same result would be obtained if we took which is 4° 57 exactly by which vertical diameter is diminished However this diminution does not occur often Therefore however it will only happen when sun's diameter diminished by about 4° 57 Hence there no considerable quantity refraction but when this angle exceeds 4° 57 The opposite result will not differ sensibly from circle Q.e.d Q.e.p Q.e.q Q.e.r Q.e.s Q.e.t Q.e.u Q.e.v Q.e.w Q.e.x Q.e.y Q.e.z Parallax. 117 Parallax consists two observations object seen at different times and places being made same instant time different distances object one place near or upon center and other far from Let C figure represent star C center earth C' center planet or satellite great distance earth's distance angle ZAC but not so far as ZAC" and let AC' nearer C than AC" Then now we know from principles trigonometry that \[ \sin CA'C \sin ZAC' = \sin ZAC'' \sin ZAC'' \] where \(\sin ZAC'' = \sin ZAC' + \sin ZAC'\) since \(ZAC'' = ZAC' + ZAC\) Consequently \[ \frac{ZAC''}{ZAC'} = \frac{\sin ZAC'' - \sin ZAC'}{\sin ZAC'} \] This formula illustrates this proposition we may see from following example In observing Venus twilight Cape Good Hope observed Mars be \(1^\circ\) \(29'\) before this month again January second last month On same day Stockholm Mars was A S T R O N O M Y. 547 Astronomy, observed to be 1° 37' 7" below the parallel of the same latitude, and at 80° 44' 36" north latitude. Hence, take $$\tan \alpha = \frac{1}{\sqrt{3}}$$ and $$\tan \beta = \frac{\sqrt{3}}{3}$$ Wherefore $c$ is $$c = \frac{1}{\sqrt{3}} + \frac{\sqrt{3}}{3} = \frac{2}{\sqrt{3}}$$ The latitude of the place being thus deter- mined, we may hence find that for the sun's rise we have an altitude of 1° 37' 7", and for its set 1° 37' 7". C. P. C. (see fig. 30) Consequently, since CA, the radius of the earth, is constant, and AB, the distance of the observer from the centre of the body, knowing therefore, the proper angle between the plane of the horizon and that of the observer, the parallax of the face of the sun will be given by the sine of this angle. This method, however, of determining the value of the parallax is not very accurate, because the measure of angles is not very exact. 189. To determine the parallax in right elevation, when the sun is at its meridian. P. F. Q. (fig. 31) Let A be the equator, B the true place, as determined by parallels in the veridical plane; C is the parallax in right elevation, and D is de- terminate by parallels in the same plane. Now $$\sin^2 x = \cos^2 Z_0 - \cos^2 Z_0$$ Hence by multiplication, and rejecting like factors, therefore $$\sin^2 x = \sin^2 Z_0$$ But $$\sin^2 x = \cos^2 Z_0$$ Therefore $$\sin^2 Z_0 = \cos^2 Z_0$$ Hence $$\sin Z_0 = \sin Z_0$$ whence by substitution $$x = Z_0$$ It follows that for the same star, where the sun is at its meridian, we have a parallax equal to the sin of twice the arc of the circle of the base angle, ABA. Also, $$\sin x = \cos Z_0$$ In the nature heavens, the apparent plane & c. on the opposite side of the earth from that on which we are situated, is called a paral- lax of $x$, and therefore for right elevation is diminished by parallel lines drawn from A to B, and other marks made, the whole change of position of the sun with respect to our sight being represented by the sum (if any) of these parts before and after the sun rises, we have $$x = \frac{1}{2} \times 360^\circ$$ So that $$x = 180^\circ$$ D. P. P. (see fig. 32) Sounding the sum of the sides of two hexagons, we have $$P_1 P_2 P_3$$ which produce to $x$, drawing the small and here $P_1$ is $\frac{1}{2}$ $P_1 P_2$ On the meridians there are no parallaxes in right elevation; but on those on which we are situated there are such, owing to the inclination of the plane when it passes the meridian; consequently, the difference between them is always equal to one half of a quadrant. If therefore we take the difference of their right ascensions, we shall have a measure of their parallaxes; but if we do not take account of this difference, we shall have a measure of their differences in longitude. This difference will be known as one half a quadrant. One observer may have more or less than another, by which a greater difference will be obtained. 190. The mean parallax in right elevation. By trans- sight, let us follow the following by means of a table: the sun's declination at noon at any time at sea, the sun's declination at noon at any time at sea, the sun's declination at noon at any time at sea, the sun's declination at noon at any time at sea, the sun's declination at noon at any time at sea, the sun's declination at noon at any time at sea, the sun's declination at noon at any time at sea, the sun's declination at noon at any time at sea, the sun's declination at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- tion at noon at any time at sea, the sun's declina- mination. At this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and at this time of observation, the distance of the moon from its perigee was 37-7 degrees; and 548 A S T R O N O M Y. Anomalous $x$ parallel to $a$, and $y$ in the perpendicular to $b$, we have the following triangles: Triangle $WZ$ $$\begin{array}{l} \text{PW} = 37^\circ 35' \\ \text{PZ} = 57^\circ 35' \\ \text{WZ} = 90^\circ - (37^\circ 35' + 57^\circ 35') = 90^\circ - 95^\circ = -5^\circ \end{array}$$ $$\text{sin } WZ = \sin (-5^\circ) = -0.08716$$ $$\text{tan } WZ = \tan (-5^\circ) = -0.08716$$ Triangle $YZ$ $$\begin{array}{l} \text{PY} = 37^\circ 35' \\ \text{PZ} = 57^\circ 35' \\ \text{YZ} = 90^\circ - (37^\circ 35' + 57^\circ 35') = 90^\circ - 95^\circ = -5^\circ \end{array}$$ $$\text{sin } YZ = \sin (-5^\circ) = -0.08716$$ $$\text{tan } YZ = \tan (-5^\circ) = -0.08716$$ Triangle $WX$ $$\begin{array}{l} \text{PW} = 37^\circ 35' \\ \text{PZ} = 57^\circ 35' \\ \text{WX} = 90^\circ - (37^\circ 35' + 57^\circ 35') = 90^\circ - 95^\circ = -5^\circ \end{array}$$ $$\text{sin } WX = \sin (-5^\circ) = -0.08716$$ $$\text{tan } WX = \tan (-5^\circ) = -0.08716$$ Triangle $WF$ $$\begin{array}{l} \text{PW} = 37^\circ 35' \\ \text{PZ} = 57^\circ 35' \\ \text{WF} = 90^\circ - (37^\circ 35' + 57^\circ 35') = 90^\circ - 95^\circ = -5^\circ \end{array}$$ $$\text{sin } WF = \sin (-5^\circ) = -0.08716$$ $$\text{tan } WF = \tan (-5^\circ) = -0.08716$$ Triangle $WF$ $$\begin{array}{l} \text{PW} = 37^\circ 35' \\ \text{PZ} = 57^\circ 35' \\ \text{WF} = 90^\circ - (37^\circ 35' + 57^\circ 35') = 90^\circ - 95^\circ = -5^\circ \end{array}$$ $$\text{sin } WF = \sin (-5^\circ) = -0.08716$$ $$\text{tan } WF = \tan (-5^\circ) = -0.08716$$ Triangle $WF$ $$\begin{array}{l} \text{PW} = 37^\circ 35' \\ \text{PZ} = 57^\circ 35' \\ \text{WF} = 90^\circ - (37^\circ 35' + 57^\circ 35') = 90^\circ - 95^\circ = -5^\circ \end{array}$$ $$\text{sin } WF = \sin (-5^\circ) = -0.08716$$ $$\text{tan } WF = \tan (-5^\circ) = -0.08716$$ Triangle $WF$ $$\begin{array}{l} \text{PW} = 37^\circ 35' \\ \text{PZ} = 57^\circ 35' \\ \text{WF} = 90^\circ - (37^\circ 35' + 57^\circ 35') = 90^\circ - 95^\circ = -5^\circ \end{array}$$ $$\text{sin } WF = \sin (-5^\circ) = -0.08716$$ $$\text{tan } WF = \tan (-5^\circ) = -0.08716$$ Triangle $WF$ $$\begin{array}{l} \text{PW} = 37^\circ 35' \\ \text{PZ} = 57^\circ 35' \\ \text{WF} = 90^\circ - (37^\circ 35' + 57^\circ 35') = 90^\circ - 95^\circ = -5^\circ \end{array}$$ $$\text{sin } WF = \sin (-5^\circ) = -0.08716$$ $$\text{tan } WF = \tan (-5^\circ) = -0.08716$$ Triangle $WF$ $$\begin{array}{l} \text{PW} = 37^\circ 35' \\ \text{PZ} = 57^\circ 35' \\ \text{WF} = 90^\circ - (37^\circ 35' + 57^\circ A S T R O N O M Y. 549 Astronomy) is in her proper and in conjunction) in 30° 27' 26" the sun's meridian, and in opposition) in 30° 27' 26" the sun's meridian, as the distance, the parallax at the mean distance of the earth from the sun, is the distance, the parallax at the mean distance of the moon from the sun. Therefore, when we have calculated the parallax from the mean distance of the earth from the sun, we shall find a slight disagreement in the two results. For, since the moon is nearer to us than the earth, its parallax must be smaller than that of the earth. But this difference between them cannot exceed 5° 57' 5" at the equator, 50° 57' 5" at the pole, and so on. Hence, if we assume that the parallax of the earth is 30° 27' 26", we may conclude that the parallax of the moon will be less than this amount by about 5° 57' 5". Assuming thus the mean parallaxes to be 30° 27' 26", we have, referring to Table I., $$\text{A} \times \text{C} = \text{D}$$ or, $$\text{A} \times \text{C} = \text{D} + \text{E}$$ where A is the mean parallax of the earth, B is that of the moon, C is their distance apart, D is their apparent diameter, and E is their actual diameter. The preceding method by which we determine the parallaxes of the sun and moon does not sufficiently serve us to employ them in deter- mining their distances. For they are both very distant bodies, and require a most important accurate element, and requires the use of a very great number of observations. In order to avoid this encumbrance, engaged the most anxious attention of everybody who has been interested in astronomy. They have offered us a most excellent service to the science than Dr. Herschel has done. He has observed with such accuracy those stars which he pointed out by the celebrated telescope. By Herschel's means we can determine with great exactness how far he compares the planetary motions to be deter- mined by their distances. For instance, let us suppose that we wish to know whether or not Mercury moves around its orbit in one year or ten years. We can easily state that it depends upon the trend of either of these two motions. If we observe Mercury for a long time over our own side and find that it has been found to move in one year, then we can say that it moves toward Lagrange; whereas we have seen (art. III.) that it moves toward Lagrange II. Therefore, we can say that Mercury moves in one year. Thus, what has been said is apparent, that the distance of any body in space is determined by its ap- pearance according to its motion. For we know how to determine their actual dis- tances directly from their motions. But for determining their distances indirectly, by means of their parallaxes, we must first ascertain whether or not their motions are uniform. If they are not uniform, we would consequently obtain all our results wrong. For example, if Mercury had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, but had moved for four million years exactly as it does now, and so forth. This can be well described in the following way: If a particle of light be at A in the telescope and be reflected back at B in the telescope so that a particle of light will be at C in the telescope and be reflected back at D in the telescope so that a particle of light will be at E in 530 # ASTRONOMY. **Astronomy** **Distance** of the *earth*, the place measured by the *sun's* diameter, is 97,000,000 miles. The distance of the *moon* is 216,000 miles. The distance of the *mercury* is 38,000 miles. The distance of the *venus* is 67,000 miles. The distance of the *mars* is 144,000 miles. The distance of the *jupiter* is 486,000 miles. The distance of the *saturn* is 1,284,000 miles. Hence it appears, that if we take the diameter of the earth, join $3\frac{1}{2}$ and complete the polygonal figure F G H I J K L M N O P Q R S T U V W X Y Z, and measure the space between any two points on the plane of the earth and the place measured by the sun's diameter, we shall find that this space is equal to the diameter of the earth at that point. Hence it follows, that if we take any other point on the plane of the object as we have done in the preceding figures, and measure its distance from the sun's diameter, we shall find that this distance will be equal to the diameter of that object at that point. The place measured by the sun's diameter being thus found, we can easily determine how far we are from any other object which has a similar diameter. For instance, if we suppose that we are in a room with a window, and that we wish to know how far away is another room with a window. We must first measure the diameter of our own room and then measure the diameter of the other room. If these diameters are equal, then we are equally distant from both rooms. If we desire to know how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then we are equally distant from both objects. In order to determine how far away is another object which has a similar diameter, we must first measure its diameter and then measure its distance from us. If these diameters are equal, then # ASTRONOMY. The star which is subject to the effect of the sun's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the sun itself. But when the star is situated at a great distance from the sun, and consequently does not receive any direct rays from it, it will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the moon itself. The star which is subject to the effect of the moon's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the moon itself. The star which is subject to the effect of the earth's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the earth itself. The star which is subject to the effect of the sun's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the sun itself. The star which is subject to the effect of the moon's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the moon itself. The star which is subject to the effect of the earth's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the earth itself. The star which is subject to the effect of the sun's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the sun itself. The star which is subject to the effect of the moon's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the moon itself. The star which is subject to the effect of the earth's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the earth itself. The star which is subject to the effect of the sun's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the sun itself. The star which is subject to the effect of the moon's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the moon itself. The star which is subject to the effect of the earth's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the earth itself. The star which is subject to the effect of the sun's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the sun itself. The star which is subject to the effect of the moon's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the moon itself. The star which is subject to the effect of the earth's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the earth itself. The star which is subject to the effect of the sun's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the sun itself. The star which is subject to the effect of the moon's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the moon itself. The star which is subject to the effect of the earth's light, will appear to us as a point of light, and we shall not be able to distinguish its place in the heavens from that of the earth itself. The star which is subject to
Astronomy.
Table - continued
Degree 6 VIL 1 VIL VII 8 VIL Degree Place Longitude
0 7950 123° 100° 943 54
1 7950 -139° 791 33
2 7950 -139° 791 33
3 7950
**Explanation:** The table provides astronomical data for various degrees of longitude, specifically for the first quadrant (from 0 to 90 degrees). Each row represents a degree, with columns indicating different celestial elements such as declination, right ascension, and other related values. - **Declination**: This column shows the declination angle for each degree. - **Right Ascension**: This column shows the right ascension angle for each degree. - **Other Values**: These columns show additional astronomical data, such as parallax, which is a measure of how much an object appears to move when viewed from slightly different positions. The table is structured in a way that allows for easy reference to specific degrees and their corresponding astronomical values. For example, to find the declination for a degree between 79° and 80°, one would look at the row corresponding to that degree and read off the declination value. This table is useful for astronomers and astrophysicists who need precise measurements of celestial objects' positions and orientations. It helps in calculating various astronomical phenomena, such as the apparent motion of stars across the sky, the position of planets relative to the Earth's surface, and other related calculations. ASTRONOMY. 553 Among peculiarities to Pt. Pk. Now, as said, the being fixed in the preceding table, is not so much a peculiarity as a general rule, which alone shows how many stars are given, complete the sum of all the planets found. Then again, as $x_0 = 0$, we have $x_0 = x_0$; as $x_0 = 1$, we have $x_0 = x_0$; as $x_0 = 2$, we have $x_0 = x_0$; as $x_0 = 3$, we have $x_0 = x_0$; as $x_0 = 4$, we have $x_0 = x_0$; as $x_0 = 5$, we have $x_0 = x_0$; as $x_0 = 6$, we have $x_0 = x_0$; as $x_0 = 7$, we have $x_0 = x_0$; as $x_0 = 8$, we have $x_0 = x_0$; as $x_0 = 9$, we have $x_0 = x_0$; as $x_0 = 10$, we have $x_0 = x_0$; as $x_0 = 11$, we have $x_0 = x_0$; as $x_0 = 12$, we have $x_0 = x_0$; as $x_0 = 13$, we have $x_0 = x_0$; as $x_0 = 14$, we have $x_0 = x_0$; as $x_0 = 15$, we have $x_0 = x_0$; as $x_0 = 16$, we have $x_0 = x_0$; as $x_0 = 17$, we have $x_0 = x_0$; as $x_0 = 18$, we have $x_0 = x_0$; as $x_0 = 19$, we have $x_0 = x_0$; as $x_0 = 20$, we have $x_0 = x_0$; as $x_0 = 21$, we have $x_0 = x_0$; as $x_0 = 22$, we have $x_0 = x_0$; as $x_0 = 23$, we have $x_0 = x_0$; as $x_0 = 24$, we have $x_0 = x_0$; as $x_0 = 25$, we have $x_0 = x_0$; as $x_0 = 26$, we have $x_0 = x_0$; as $x_0 = 27$, we have $x_0 = x_0$; as $x_0 = 28$, we have $x_0 = x_0$; as $x_0 = 29$, we have $x_0 = x_0$; as $x_0 = 30$, we have $x_0 = x_0$; as $x_0 = 31$, we have $x_0 = x_0$; as $x_0 = 32$, we have $x_0 = x_0$; as $x_0 = 33$, we have $x_0 = x_o # ASTRONOMY. 534 **Astronomy.** **Use of the Tables** For the above table of variation, enter Table I with the argument $A = 0$, and Table II with a $B = 0$. Then sum the two terms of the first column of Table I, which will be the information in right ascension. Enter Table I, with the argument $A = 8$ & 3.6, and Table II, with a $B = 8$ & 3.6, then sum the two corresponding numbers multiplied by the star's $\alpha$ and $\delta$ respectively, to obtain the value of the variation. Enter Table III, with the arguments $C = D$ and $E = F$, by which will be found the other two parts of the equation (the second term), which will give the whole of the alteration in declination. The third term is obtained by adding together all six signs of the second column of Table I, and dividing by the increments $D + D - D$. Humboldt on Jupiter Required the observation of a Jupiter. Feb. 15, 1839. Hereby is given a table of variations for Jupiter.
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