Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002pasj...54..493f&link_type=abstract
Publications of the Astronomical Society of Japan, Vol.54, No.3, pp.493-499
Astronomy and Astrophysics
Astronomy
1
Celestial Mechanics, Kuiper Belt, Solar System: Formation
Scientific paper
A mean motion resonance with Neptune is one of the major dynamical characteristics of the Edgeworth-Kuiper Belt Objects that spread over the outside of Neptune's orbit. We investigated the influence of Jupiter, Saturn, and Uranus on the dynamical structure of the 2 : 3 mean motion resonance with Neptune. Since the distance between the planets and objects has great influence on the dynamical structure, numerical integrations were carried out for test particles for 5Myr under five fictitious solar-system models having different configurations. In discussion about the results, we concentrate on the size of the EKBO eccentricities, e, because they have an especially close relation to the orbital evolution; for example, larger e, objects have more opportunities to encounter other objects or planets. By comparing the results of each model, it was found that the resonance structure is not largely affected by Jupiter and Saturn, and that the largest e of the resonant objects depends on the distance between Uranus and the resonance. The distance also influences the structure around the resonance because of variation in the secular resonance positions. We further found that the largest e values of the non-resonant objects at each semi-major axis do not depend on the distance from Uranus; however, they depend on the distance from Neptune.
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