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Hill Stability in the Full 3-Body Problem

Published online by Cambridge University Press:  05 January 2015

D. J. Scheeres
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Abstract

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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.

Keywords

celestial mechanicsmethods: analytical3-body problemHill stability
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S310: Complex Planetary Systems , July 2014 , pp. 134 - 137
Copyright
Copyright © International Astronomical Union 2014 

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