Astronomical Tables and Formulæ Together with a Variety of Problems Explanatory of Their Use and Application: To which are Prefixed the Elements of the Solar System ...

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R. Taylor, 1827 - 267 pages

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Page 20 - from two causes: 1° the unequal motion of the earth in its orbit; 2° the obliquity of that orbit to the plane of the equator. The mean and apparent solar days are never equal, except when the sun's daily motion in right ascension is equal to 59'. 8",33.
Page 31 - Its orbit is inclined to the plane of the ecliptic, in an angle of 7°. 8'. 9": which, according to M. Santini, has an annual decrease of 0", 12. Its ascending node -was, on January 1, 1820, in 103°. 13'.
Page 6 - to the times employed in describing them. 3°. The squares of the times of the sidereal revolutions of the planets are to each other as the cubes of their mean distances. the
Page 6 - 1°. The orbit of each planet is an ellipse; of which the sun occupies one of the foci. 2°. The areas described about the sun, by the radius vector of the planet, are proportional to the times employed in describing them.
Page 45 - the same time as the tropical revolution in her orbit: whence she always presents nearly the same face to the earth. But, as the motion of the moon, in her orbit, is periodically variable, we sometimes see more of her eastern edge, and sometimes more of her western edge. This appearance is called
Page 41 - The squares of the times of the revolutions of the satellites, round their respective primary planets, are to each other as the cubes of their mean distances from the
Page 7 - The radius vector is an imaginary line drawn from the centre of the sun, to the centre of the planet, in any part of its orbit. The
Page 76 - L = the Latitude of the place of observation: (minus, when South) D = the Declination, at the time of noon, on the given day: (minus, when South) 8 = the double daily variation in the declination, deduced from the noon of the preceding day to the noon of the following day : (minus, when the sun is
Page 55 - that, for a great number of years at least, the first three satellites cannot be eclipsed at the same time. For, in the simultaneous eclipses of the second and third, the first will always be in conjunction with Jupiter : and vice versa.
Page 55 - of the second. And the mean sidereal or synodical longitude of the first, minus three times that of the second, plus twice that of the third, is

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