On the Stability of Co-orbital Motion with Jupiter, Saturn, Uranus and Neptune

Details On the Stability of Co-orbital Motion with Jupiter, Saturn, Uranus and Neptune On the Stability of Co-orbital Motion with Jupiter, Saturn, Uranus and Neptune

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000dps....32.1902n&link_type=abstract

American Astronomical Society, DPS Meeting #32, #19.02; Bulletin of the American Astronomical Society, Vol. 32, p.1027

Astronomy and Astrophysics

Astronomy

1

Scientific paper

A systematic numerical search for stable co-orbital motion with the outer planets is presented. It is shown that the motion near triangular Lagrangian points (tadpole orbits) of all outer planets except Saturn, is stable over the age of the solar system, assuming the present configuration of planetary orbits. The low-amplitude tadpole orbits with Saturn are strongly unstable due to the overlap between two mean motion resonances: the exterior 2:5 with Jupiter and the 1:1 with Saturn. This fact is demonstrated by computing the surfaces of section in the model with Jupiter and Saturn on circular co-planar orbits. We discuss the consequences of the mean motion resonances overlap on the primordial population of Trojan-type asteroids at the stage of planetary migration. This research was sponsored by CNRS.

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