Analytic perturbation solutions to the Venusian orbiter due to the nonspherical gravitational potential
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The analytic perturbation solutions to the motions of a planetary orbiter given in this paper are effective for 0e1, where e is the orbital eccentricity of the orbiter. In the solution, it is assumed that the rotation of the central body is slow, and its astronomical background is clear. Examples for such planets in the solar system are Venus and Mercury. The perturbation solution is tested numerically on two Venusian orbiters with eccentric orbits, PVO and Magellan, and found to be effective.
Keywordsslow rotation central body Venusian orbiter nonspherical gravitational potential analytic perturbation solutions.
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