Hill Stability in the Full 3-Body Problem
Abstract
Hill stability cannot be easily established in the classical 3-body problem with point masses, as sufficient energy for escape of one of the bodies can always be extracted from the gravitational potential energy. For the finite density, so-called Full 3-body problem the lower limits on the gravitational potential energy ensure that Hill stability can exist. For the equal mass Full 3-body problem this can be easily established, with the result that for any equal mass, finite density 3-body problem in or near a contact equilibrium, none of the components of the system can escape in the ensuing motion.
- Publication:
-
Complex Planetary Systems, Proceedings of the International Astronomical Union
- Pub Date:
- July 2014
- DOI:
- 10.1017/S1743921314008047
- Bibcode:
- 2014IAUS..310..134S
- Keywords:
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- celestial mechanics;
- methods: analytical;
- 3-body problem;
- Hill stability