Motion near the 3/1 resonance of the planar elliptic restricted three body problem

Details Motion near the 3/1 resonance of the planar elliptic restricted three body problem Motion near the 3/1 resonance of the planar elliptic restricted three body problem

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989cemda..47...99h&link_type=abstract

Celestial Mechanics and Dynamical Astronomy, Volume 47, Issue 2, pp.99-121

Astronomy and Astrophysics

Astronomy

1

Resonance, Kirkwood Gaps, Perturbation Method, Chaotic Motion, Secondary Resonance

Scientific paper

The global semi-numerical perturbation method proposed by Henrard and Lemaître (1986) for the 2/1 resonance of the planar elliptic restricted three body problem is applied to the 3/1 resonance and is compared with Wisdom's perturbative treatment (1985) of the same problem. It appears that the two methods are comparable in their ability to reproduce the results of numerical integration especially in what concerns the shape and area of chaotic domains. As the global semi-numerical perturbation method is easily adapted to more general types of perturbations, it is hoped that it can serve as the basis for the analysis of more refined models of asteroidal motion. We point out in our analysis that Wisdom's uncertainty zone mechanism for generating chaotic domains (also analysed by Escande 1985 under the name of slow Hamiltonian chaotic layer) is not the only one at work in this problem. The secondary resonance ω p = 0 plays also its role which is qualitatively (if not quantitatively) important as it is closely associated with the random jumps between a high eccentricity mode and a low eccentricity mode.

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