A survey of the motions of asteroids in the commensurabilities with Jupiter

Details A survey of the motions of asteroids in the commensurabilities with Jupiter A survey of the motions of asteroids in the commensurabilities with Jupiter

Apr 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...213..436y&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 213, no. 1-2, April 1989, p. 436-458.

Astronomy and Astrophysics

Astronomy

65

Asteroids, Jupiter (Planet), Orbital Resonances (Celestial Mechanics), Perturbation Theory, Solar Orbits, Eccentric Orbits, Four Body Problem, Saturn (Planet), Secular Variations, Jupiter, Asteroids, Motion, Celestial Mechanics, Resonance, Astronomy, Kirkwood Gaps, Perturbations, Gravity Effects, Numerical Methods, Models, Simulations, Eccentricity, Calculations, Analysis, Procedure, Origin, Orbital Elements, Distribution, Hypotheses, Formation, Orbits, Dynamics

Scientific paper

The eccentricity variations of real and fictitious asteroids in 28 mean motion resonances with Jupiter were investigated using a semianalytical model and numerical integrations. The positions of resonances were calculated by the Kepler's third law. Results indicate that, in resonances that correspond to the Kirkwood gaps (3:1, 5:2, 7:3, and 2:1), the eccentricities of some fictitious asteroids may become 0.4 or larger. On the contrary, the eccentricities of real asteroids which belong to one of the groups (3:2, 4:3, and 1:1) remain small. Results support the following hypotheses about the origin of the gaps (or depleted regions) and the groups: (1) asteroids were removed from the resonances that correspond to the gaps by the close encounters with major planets which occurred when the eccentricities of asteroids became large, and (2) in the outer region of the main belt, asteroids have remained in some particular resonances where close encounters with Jupiter can be avoided.

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