Abstract
Stability conditions are established in the problem of two gravitationally interacting rigid bodies, designated here as the full two-body problem. The stability conditions are derived using basic principles from the N-body problem which can be carried over to the full two-body problem. Sufficient conditions for Hill stability and instability, and for stability against impact are derived. The analysis is applicable to binary small-body systems such as have been found recently for asteroids and Kuiper belt objects.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Maciejewski, A. J.: 1995, 'Reduction, relative equilibria and potential in the two rigid bodies problem', Celest. Mech. & Dyn. Astr. 63, 1-28.
MacMillan, W. D.: 1960, Dynamics of Rigid Bodies, Dover.
Pollard, H.: 1976, Celestial Mechanics, Carus Mathematical Monographs, Number 18, The Mathematical Association of America.
Scheeres, D. J., Ostro, S. J., Werner, R. A., Asphaug, E. and Hudson, R. S.: 2000, 'Effects of gravitational interactions on asteroid spin states', Icarus 147, 106-118.
Scheeres, D. J.: 2001, 'Changes in rotational angular momentum due to gravitational interactions between two finite bodies', Celest. Mech. & Dyn. Astr. 81, 39-44.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Scheeres, D.J. Stability in the Full Two-Body Problem. Celestial Mechanics and Dynamical Astronomy 83, 155–169 (2002). https://doi.org/10.1023/A:1020143116091
Issue Date:
DOI: https://doi.org/10.1023/A:1020143116091