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Issue A&A
Volume 405, Number 3, July III 2003
Page(s) 1145 - 1151
Section The Sun
DOI http://dx.doi.org/10.1051/0004-6361:20030654



A&A 405, 1145-1151 (2003)
DOI: 10.1051/0004-6361:20030654

The resonant dynamical evolution of small body orbits among giant planets

R. Gabryszewski1 and I. Wlodarczyk2

1  Space Research Centre, ul. Bartycka 18A, 00-716 Warszawa, Poland
    e-mail: r.gabryszewski@cbk.waw.pl
2  Astronomical Observatory of the Chorzów Planetarium, WPKiW, 41-501 Chorzów, Poland
    e-mail: astrobit@ka.onet.pl

(Received 15 January 2003 / Accepted 25 April 2003)

Abstract
Mean motion resonances (MMRs) can lead either to chaotic or regular motion. We report on a numerical experiment showing that even in one of the most chaotic regions of the Solar System - the region of the giant planets, there are numerous bands where MMRs can stabilize orbits of small bodies in a time span comparable to their lifetimes. Two types of temporary stabilization were observed: short period (~ 104 years) when a body was in a MMR with only one planet and long period (over  105 years) when a body is located in overlapping MMRs with two or three planets.

The experiment showed that the Main Belt region can be enriched by cometary material in its pre-active state due to temporary resonant interactions between small bodies and giant planets.


Key words: solar system: general -- minor planets, asteroids -- celestial mechanics

Offprint request: R. Gabryszewski, r.gabryszewski@cbk.waw.pl




© ESO 2003


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