Core instability models of giant planet accretion – II. Forming planetary systems

Y. MIGUEL, AND A. BRUNINI

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

WILEY-BLACKWELL PUBLISHING, INC

Año: 2009 vol. 392 p. 391 - 399

0035-8711

We develop a simple model for computing planetary formation based on the core instabilitymodel for the gas accretion and the oligarchic growth regime for the accretion of the solid core.In this model several planets can form simultaneously in the disc, a fact that has importantimplications especially for the changes in the dynamic of the planetesimals and the growthof the cores since we consider the collision between them as a source of potential growth.The type I and type II migration of the embryos and the migration of the planetesimalsdue to the interaction with the disc of gas are also taken into account. With this model weconsider different initial conditions to generate a variety of planetary systems and analyse themstatistically.We explore the effects of using different type I migration rates on the final numberof planets formed per planetary system such as on the distribution of masses and semimajoraxis of extrasolar planets, where we also analyse the implications of considering differentgas accretion rates. A particularly interesting result is the generation of a larger population ofhabitable planets when the gas accretion rate and type I migration are slower.