Long-term evolution of the asteroid orbits at the 3:1 mean motion resonance with Jupiter (planar problem)

Abstract

The 3:1 mean-motion resonance of the planar elliptic restricted three body problem (Sun-Jupiter-asteroid) is considered. The double numeric averaging is used to obtain the evolutionary equations which describe the long-term behavior of the asteroid's argument of pericentre and eccentricity. The existence of the adiabatic chaos area in the system's phase space is shown.

17 pages, 20 figures

References in corpus (1)

• Could the 55 Cancri Planetary System Really Be in the 3:1 Mean Motion Resonance?

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