Lines Matching full:sun
95 * it takes for the moon to return the same ecliptic longitude as the sun.
96 * It is longer than the sidereal month because the sun's longitude increases
97 * during the year due to the revolution of the earth around the sun.
111 * the revolution of the earth around the sun.
134 * for the sun to return to the same position against the fixed stellar
135 * background. This is the duration of one orbit of the earth about the sun
522 // The Sun
526 // Parameters of the Sun's orbit as of the epoch Jan 0.0 1990
537 // The following three methods, which compute the sun parameters
547 // * Return the sun's ecliptic longitude at perigee for the current time.
557 // * Return the sun's ecliptic longitude for the current time.
573 // * Return the sun's eccentricity of orbit for the current time.
612 * The longitude of the sun at the time specified by this object.
618 * equation for the earth and the sun. It does not take into account the
644 // Find the angular distance the sun in a fictitious
648 // The epoch wasn't at the sun's perigee; find the angular distance
660 * The position of the sun at this object's current date and time,
717 * Find the next time at which the sun's ecliptic longitude will have
768 // // Alternate Sun Rise/Set
777 // // 1. Calculate coordinates of the sun's center for midnight
829 // // 9. Correct for parallax, refraction, and sun's diameter
896 // // Alternate Sun Rise/Set
921 // // COMPUTING THE SUN'S POSITION
924 // // To be able to compute the Sun's rise/set times, you need to be able to
925 // // compute the Sun's position at any time. First compute the "day
935 // // the Sun's apparent orbit (i.e., really the Earth's orbit): w =
955 // // The Sun's true longitude, slon, can now be computed:
959 // // Since the Sun is always at the ecliptic (or at least very very close to
960 // // it), we can use simplified formulae to convert slon (the Sun's ecliptic
961 // // longitude) to sRA and sDec (the Sun's RA and Dec):
993 // // add 360 deg to MT. If the object is the Sun, leave the time as it is,
1009 // // for the Sun's upper limb, set h0 = -50/60 (-50 arc minutes).
1017 // // When HA0 has been computed, leave it as it is for the Sun but multiply
1027 // // need a quick result, check the USNO's Sun or Moon Rise/Set Table,
1083 // Evection: the sun's gravity affects the moon's eccentricity
1084 // Annual Eqn: variation in the effect due to earth-sun distance
1108 // And finally, find the variation, caused by the fact that the sun's
1142 * current ecliptic longitudes of the sun and the moon,
1325 // Sun Jul 22 10:57:41 CST 1990
1331 // newMoon(7507(Sun Jul 22 00:00:00 CST 1990,false))=
1332 // Sun Jul 08 13:56:15 CST 1990
