Astronomy and Astrophysics – Astronomy
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dda....40.0204c&link_type=abstract
American Astronomical Society, DDA meeting #40, #2.04; Bulletin of the American Astronomical Society, Vol. 41, p.895
Astronomy and Astrophysics
Astronomy
Scientific paper
Planetesimal-driven migration has been shown to be an important dynamical mechanism for the formation of giant planet cores (Levison, Thommes & Duncan, in preparation); indeed this migration rate (Kirsh et al., 2009) is faster than nominal tidally-induced migration rates in gas disks (e.g., Type - I migration) for cores less than a few Earth masses. Our earlier work (Capobianco, Duncan and Levison, in preparation) neglected Type - I tidal torquing but included a prescription for aerodynamic gas drag (Adachi et al., 1976) on a population of equal-sized planetesimals. We demonstrated that the migration of cores in minimum mass solar nebulae can be self-sustaining in either the inward or outward direction. Outward migration is easily triggered and favoured only for a plausible (albeit narrow) range of planetesimal radii 1.0 km. This outward migration can be accompanied by substantial mass accretion.
We have now included a prescription for Type - I orbital migration (Papaloizou & Larwood, 2000) for the giant planet cores, as well as a planetesimal size spectrum to mimic a collisional cascade. Our results indicate that the dynamics of the cores will be dominated by the planetesimals in the size range containing most of the mass of the planetesimal population. The inclusion of Type - I migration modifies our results for the tendency for outward versus inward migration, but surprisingly we find that, once initiated, outward migration of the cores can be maintained despite the presence of inward Type - I torquing.
Capobianco Christopher
Duncan Martin J.
Levison Harold F.
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