Structure of the 2:1 and 3:2 Jovian resonances

Details Structure of the 2:1 and 3:2 Jovian resonances Structure of the 2:1 and 3:2 Jovian resonances

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986icar...65...70m&link_type=abstract

Icarus (ISSN 0019-1035), vol. 65, Jan. 1986, p. 70-82.

Physics

80

Asteroids, Eccentric Orbits, Jupiter (Planet), Resonance, Three Body Problem, Celestial Mechanics, Chaos, Convergence, Phase-Space Integral, Series Expansion, Jupiter, Structure, Resonance, Mapping, Techniques, Celestial Mechanics, Eccentricity, Asteroids, Orbits, Hilda Asteroids, Position (Location), Kirkwood Gaps, Hecuba Gap

Scientific paper

The chaotic regions of the phase space in the vicinity of the 2:1 and 3:2 jovian resonances are identified by using a mapping technique derived from a second-order expansion of the disturbing function for the planar elliptical restricted three-body problem. It is shown that both resonances have extensive chaotic regions which in some cases can lead to large changes in the eccentricity of asteroid orbits. Although the 3:2 resonance is shown to be more chaotic than the 2:1 resonance, the existence of the Hilda group of asteroids and the Hecuba gap may be explained by distinct differences in the location of the high-eccentricity regions at each resonance. The problem of the convergence of the expansion of the disturbing function in the outer asteroid belt is also discussed.

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