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Retrograde motion in astronomy is, in general, orbital or rotational motion of an object in the direction opposite the rotation of its primary, that is, the central object (right figure). It may also describe other motions such as precession or nutation of an object's rotational axis .
The retrograde motion of a hypothetical extremely distant (and nearly non-moving) planet would take place during a half-year, with the planet's apparent yearly motion being reduced to a parallax ellipse. The center of the retrograde motion occurs at the planet's opposition which is when the planet is exactly opposite the Sun.
Vakragati means retrograde motion. As the Earth passes by a planet that particular planet appears to move backwards i.e. westward, amid the stars, this phenomenon is called retrograde motion, which motion invariably occurs at a time when that planet is visible for a relatively longer period. the approximate midpoint of which period in respect of the superior planets coincides with opposition ...
When Neptune, planet of illusion, is in direct motion, we can be confused by our sentiments and emotions. When it is retrograde, the veil is lifted, and we can sort through our feelings.
A satellite with an orbital inclination between 90° and 180° (or, equivalently, between 0° and −90°) is said to be in a retrograde orbit. [note 2] A satellite in a direct orbit with an orbital period less than one day will tend to move from west to east along its ground track. This is called "apparent direct" motion.
Planets moving in direct motion, aka non-retrograde planets, act in a very predictable way without much fuss or fanfare. Most of the time, planets move in this forward motion, and things carry on ...
At the equator, the solar rotation period is 24.47 days. This is called the sidereal rotation period, and should not be confused with the synodic rotation period of 26.24 days, which is the time for a fixed feature on the Sun to rotate to the same apparent position as viewed from Earth (the Earth's orbital rotation is in the same direction as the Sun's rotation).
The Sun-centered positions displayed a cyclical motion with respect to time but without retrograde loops in the case of the outer planets. [dubious – discuss] In principle, the heliocentric motion was simpler but with new subtleties due to the yet-to-be-discovered elliptical shape of the orbits. Another complication was caused by a problem ...