Physics
Scientific paper
Mar 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..marh33090p&link_type=abstract
American Physical Society, Annual APS March Meeting, March 18 - 22, 2002 Indiana Convention Center; Indianapolis, Indiana Meetin
Physics
Scientific paper
Recent research has suggested compelling evidence that the outer Jovian planets, Uranus and Neptune, may have formed much closer to the sun then they are now. Computer simulations of planetary growth have shown that they may have formed in the Jupiter-Saturn region of the solar system (4-10AU). If this is the case, then somehow the ice planets (Uranus and Neptune) have migrated outwards to their current location. The most likely mechanism for achieving this kind of orbital migration is a close encounter with a large planet, most likely Jupiter itself. However this encounter would have thrown the smaller planet outwards with a large eccentricity and possibly a large inclination to the orbital plane. Somehow this eccentricity and inclination must have been reduced to the current orbits and in Uranus’ case, a near perfectly circular orbit. Using the SWIFT orbital integration software and some recent modifications, I have attempted to show that relatively high eccentricities can be “damped out” by interactions with the dust and gas present in the early solar nebula when this migration must have occurred.
Perkins Michael
Williams Darren
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