Què opinen els usuaris - Escriviu una ressenya
No hem trobat cap ressenya als llocs habituals.
Altres edicions - Mostra-ho tot
aberration altitude angular apogee apparent diameter apparent place argument of latitude ascension and declination azimuth called clock conjunction consequently corresponding declination circle described determined direction disk diurnal circle Earth Earth's axis Earth's center Earth's surface ecliptic equal equator equinox error fixed stars geocentric greatest heavenly body heavens heliocentric Hence horizon hour angle inclination inferior planet intersection interval Jupiter known latitude and longitude length line joining lunar lunar eclipse mean distance meridian zenith distance nearly node north polar distance nutation obliquity observed parallax parallel passing perigee perihelion perpendicular plane point of Aries pole position precession radius vector refraction right ascension rotation round satellite seen semi-diameter shadow sidereal sidereal day sidereal period sin2 solar eclipse solstice star's Sun and Moon Sun's center Sun's declination supposed tangent telescope tion transit triangle true true anomaly values velocity Venus vertical visible zenith distance
Pàgina 55 - The third, viz. that the squares of the periodic times are proportional to the cubes of the mean distances...
Pàgina 264 - If the mean angular velocity of the first satellite be added to twice that of the third, the sum will be equal to three times that of the second ;" and "from this it results that the situations of any two of them being given, that of the third can be found.
Pàgina 81 - An account of experiments for determining the length of the pendulum vibrating seconds in the latitude of London.
Pàgina 16 - IV. The ecliptic and its pole may be taken as the standards of reference. The co-ordinates of the star are then called its latitude and its longitude. The Latitude of a star is its angular distance from the ecliptic measured on a circle of latitude. The Longitude of a star is the arc of the ecliptic included between the vernal equinox and the point where the circle of latitude through the star cuts the ecliptic.
Pàgina 137 - Wollaston concludes, that all the phenomena accord entirely with the supposition that the Earths atmosphere is of finite extent, limited by the weight of ultimate atoms, of definite magnitude, no longer divisible by repulsion of their parts.
Pàgina 293 - The greatest number of eclipses that can happen in a year is seven; five of the sun and two of the moon, or four of the sun and three of the moon.
Pàgina 114 - B . sin c = sin b . sin C cos a = cos b . cos c + sin b . sin c cos b = cos a . cos c + sin a . sin c cos A cos B cos c = cos a . cos b + sin a . sin b . cos C ..2), cotg b . sin c = cos G.
Pàgina 312 - Time, the angular distances between the apparent centres of the Moon and certain heavenly bodies, such as they would appear to an observer at the centre of the Earth. When a Lunar Distance has been observed on the surface of the Earth, and reduced to the centre, by clearing it of the effects of parallax and refraction, the numbers...
Pàgina 55 - Sun, moves from west to east ; or according to the order of the signs, or, as the phrase may still be varied, in consequentia.
Pàgina 48 - NODE, (1) in astronomy, the two points in which the orbit of a planet intersects the plane of the ecliptic; the one through which the planet passes from the south to the north side of the ecliptic being called the ascending node, and the other the descending node. As all the bodies of the solar system, whether planets or comets, move in orbits variously inclined to the ecliptic, the orbit of each possesses two nodes, and a straight line drawn joining these two points is called the line of nodes of...