The Hill stability of planetary motion under stellar approaches
Abstract
A planetary motion under the influence of a star passing near the Solar system is examined in the framework of the three-dimensional restricted three-body problem. The exact expression of the force function without expansion it in series is used. An integral invariant relation - quasi-integral - is found, and regions of possible motion of a passively gravitating body are determined. Surfaces of minimal energy which are generalizations of surfaces of zero velocity are plotted. The Hill stability of planetary motion is investigated when a star with a mass between one and five solar masses approaches the Solar system at a minimum distance of 50 AU up to 100 AU. The results obtained are shown in the form of tables. Refs 10. Tables 2.
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Articles of "Vestnik of Saint Petersburg University. Mathematics. Mechanics. Astronomy" are open access distributed under the terms of the License Agreement with Saint Petersburg State University, which permits to the authors unrestricted distribution and self-archiving free of charge.