Extended core accretion models

Details Extended core accretion models Extended core accretion models

Feb 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006tafp.conf...13a&link_type=abstract

"Tenth Anniversary of 51 Peg-b: Status of and prospects for hot Jupiter studies. Colloquium held at Observatoire de Haute Proven

Computer Science

Scientific paper

We present our extended core accretion models of giant planet formation, including migration and disk evolution. We show that taking these effects into account can lead to much more rapid formation of giant planets, making it compatible with the typical disk lifetimes inferred from observations of young circumstellar disks. We apply these models to the formation of our own solar system, and show that they can account for both the internal structure of the two planets, as derived by Saumon & Guillot (2004, ApJ 609, 1170-1180), and the atmospheric abundance of some volatile elements measured in situ by the Galileo probe or by remote sensing. We finally present a consistent scenario combining formation and evolutionary models aimed at explaining the existence of a hot-Neptune in μ Ara-like systems. We show that a planet forming through our extended core accretion model and undergoing evaporation provides a suitable explanation for this type of light planets.

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