Accretion of Cores of the Giant Planets

Details Accretion of Cores of the Giant Planets Accretion of Cores of the Giant Planets

Mar 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004pfte.confe..30w&link_type=abstract

Presented at the KITP Conference: Planet Formation: Terrestrial and Extra Solar, Mar 18, 2004, Kavli Institute for Theoretical P

Physics

Scientific paper

Accretion in the outer solar nebula differs from the terrestrialplanet region, due to lower orbital velocities and larger massesof the first planetary embryos that form. The first "oligarchic"embryos that grow beyond the "snow line" can scatter smaller bodiesoutward. These scattered bodies have their orbits circularizedin the outer nebula by dynamical friction. As they are much moremassive than the indigenous planetesimals, they can act as seedbodies for rapid runaway growth. The scattering process impliesthat the number and orbital spacing of outer planets are stochasticrather than deterministic.

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