Forming Giant Planets in the Face of Migration

Details Forming Giant Planets in the Face of Migration Forming Giant Planets in the Face of Migration

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.6306c&link_type=abstract

American Astronomical Society, DPS meeting #38, #63.06; Bulletin of the American Astronomical Society, Vol. 38, p.611

Astronomy and Astrophysics

Astronomy

Scientific paper

Planetary migration poses a serious problem for theories of planet formation. In the core accretion model, giant planets form a solid core of roughly 10 Earth masses by accumulating from planetesimals. The core subsequently accretes a gaseous envelope. Cores generate and interact with spiral density waves in the nebula gas, moving inwards via type-I migration. Larger bodies clear a gap in the disk and follow the gas's viscous accretion, moving inwards via type-II migration. The time required to form a 10-Earth-mass core is roughly 1 million years in most models, which is much longer than the 10,000 to 30,000 year lifetime of the core against type-I migration. Protoplanetary disks last for several million years, which is longer than the lifetime of a giant planet with respect to type-II migration for typically considered values of the disk viscosity parameter alpha.
Here I will describe results of a new model for planetary formation and migration. I will show that gas-giant planets can form and survive both type-I and type-II migration under certain conditions. Under these conditions, a protoplanetary disk a few times more massive than the Sun's minimum-mass nebula naturally gives rise to a system of giant planets like those in the Solar System. Different values of the model parameters give rise to giant planets at a range of orbital distances from their formation location to the inner edge of the disk. This is similar to the observed orbital distribution of extrasolar planets.
This work was supported by NASA's Terrestrial Planet Finder Foundation Science research programme.

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