Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...275..301v&link_type=abstract
Astronomy and Astrophysics, Vol. 275, p. 301 (1993)
Astronomy and Astrophysics
Astrophysics
2
Celestial Mechanics, Stellar Dynamics, Minor Planets
Scientific paper
In a recent work (Varvoglis 1991) we proposed the use of a model dynamical system as a fast and effective method to study the motion of asteroids in the main asteroidal belt. This dynamical system is, essentially, a modified planar elliptical restricted three-body problem, in which the variation of Jupiter's eccentricity, caused by the perturbation of Saturn, is taken explicitly into account. Here we show that, near the 2:1 resonance, the (osculating) eccentricity, e, of the trajectories of this dynamical system may attain high values (e ≥ 0.6) and that a fictitious asteroid, following such a "high-e" trajectory, may undergo a close encounter with Jupiter and be subsequently removed from the 2:1 resonance region.
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