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Kepler's equation
Orbital mechanics term / From Wikipedia, the free encyclopedia
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For specific applications of Kepler's equation, see Kepler's laws of planetary motion.
In orbital mechanics, Kepler's equation relates various geometric properties of the orbit of a body subject to a central force.
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It was derived by Johannes Kepler in 1609 in Chapter 60 of his Astronomia nova,[1][2] and in book V of his Epitome of Copernican Astronomy (1621) Kepler proposed an iterative solution to the equation.[3][4] This equation and its solution, however, first appeared in a 9th-century work by Habash al-Hasib al-Marwazi, which dealt with problems of parallax.[5][6][7][8] The equation has played an important role in the history of both physics and mathematics, particularly classical celestial mechanics.