Uranus and Neptune: Fugitives from the Jupiter-Saturn zone?

Details Uranus and Neptune: Fugitives from the Jupiter-Saturn zone? Uranus and Neptune: Fugitives from the Jupiter-Saturn zone?

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999dda....31.0102t&link_type=abstract

American Astronomical Society, DDA meeting #31, #01.02

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Scientific paper

Plantesimal accretion models of planet formation have been quite successful at reproducing the terrestrial region of the Solar System. However, in the outer Solar System these same models break down; without invoking other mechanisms, it becomes very difficult to grow bodies to the current mass of Uranus and Neptune. An alternative scenario to in-situ formation of these planets is explored here. In addition to the Jupiter and Saturn solid cores, several more bodies of mass ~ 10 MEarth are likely to have formed in the region between 5 and 10 AU. If such bodies were subsequently scattered outward, dynamical friction with the protoplanetary disk would have acted to damp their initially high eccentricites and inclinations, and could have left some of them in circular, low-inclination orbits in the outer Solar System. Numerical simulations, using a code which fully models close encounters, show this scenario to be quite plausible for reasonable protoplanetary disk surface densities.

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