Giant Planet Accretion And Migration: Surviving The Type I Regime

Details Giant Planet Accretion And Migration: Surviving The Type I Regime Giant Planet Accretion And Migration: Surviving The Type I Regime

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dda....37.0302t&link_type=abstract

American Astronomical Society, DDA meeting #37, #3.02; Bulletin of the American Astronomical Society, Vol. 38, p.667

Astronomy and Astrophysics

Astronomy

Scientific paper

In the core accretion model of gas giant planet formation, a large solid core about 10X the Earth's mass forms first, then accumulates its massive envelope ( 100 or more Earth masses) of gas. However, inward planet migration due to gravitational interaction with the proto-stellar gas disk poses a big hazard in this model. Core-sized bodies undergo rapid "type I" migration; for typical parameters their migration timescale is much shorter than their accretion timescale. How, then, do growing cores avoid spiraling into the central star before they ever get the chance to become gas giants? I will present a simple model of core formation in a gas disk which is viscously evolving. It turns out that as the disk accretes onto the star, a window of opportunity for successful core growth may open. I will discuss what implications this model has for the link between disk properties and the likelihood of forming gas giants.

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