Stability of the orbit of a third body in binary asteroid systems

Details Stability of the orbit of a third body in binary asteroid systems Stability of the orbit of a third body in binary asteroid systems

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010jphcs.218a2017n&link_type=abstract

Journal of Physics: Conference Series, Volume 218, Issue 1, pp. 012017 (2010).

Physics

Scientific paper

In this work we studied the stable regions around four binary asteroids in the main asteroid belt. The studied systems were (107) Camilla, (22) Kallipe, (45) Eugenia and (762) Pulcova. The stability was characterized with three motion indicators: relative Lyapunov indicator, maximum eccentricity, and maximum difference of eccentricities. The survay covered the P type orbits, where satellite moves around both primaries. On the basis of our work it can be decided, in which system the discovery of a third component can be expected.

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