Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.5807c&link_type=abstract
American Astronomical Society, DPS meeting #40, #58.07; Bulletin of the American Astronomical Society, Vol. 40, p.504
Astronomy and Astrophysics
Astronomy
Scientific paper
In the core-accretion model for giant-planet formation, large solid cores form via runaway and oligarchic growth from a population of small planetesimals. Once a core reaches roughly 10 Earth masses, it can begin to accrete a gaseous envelope provided that gas is still present in the protoplanetary disk. High-velocity collisions between planetesimals generate small fragments. Interactions between a core and the surrounding gas disk can cause rapid inward planetary migration. Fragmentation and migration each have positive and negative effects on the formation of giant-planet cores. Small fragments are accreted more quickly than large planetesimals, speeding up growth. However, fragments drift inwards rapidly and can be lost. Migration allows a core to grow beyond its isolation mass by moving into new regions of the disk. However, cores can also be lost if migration rates are high. Here, I will describe results of new simulations of giant-planet core formation including migration and fragmentation. I will show that fragmentation usually aids growth. Migration at nominal rates typically, but not always, prevents the formation of giant-planet cores.
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