Giant planet formation via pebble accretion

O. M. GUILERA

Paris

Congreso; 31st. International Colloquium of the Institut d?Astrophysique de Paris: From Super Earths to Brown Dwarfs: Who?s Who?; 2015

Observatorio de Paris

In the standard model of core accretion, the formation of giant planets occurs by two main processes: first, a massive core is formed by the accretion of solid material; then, whenthis core exceeds a critical value (typically greater than 10 Earth masses) a gaseous runaway growth is triggered and the planet accretes big quantities of gas in a short period oftime until the planet achieves its final mass. Thus, the formation of a massive core has to occur when the nebular gas is still available in the disk. This phenomenon imposesa strong time-scale constraint in giant planet formation due to the fact that the lifetimes of the observed protoplanetary disks are between 1 Myr and 10 Myr. The formationof massive cores before 10 Myr by accretion of big planetesimals (with radii >10 km) in the oligarchic growth regime is only possible in massive disks. However, planetesimalaccretion rates significantly increase for small bodies, especially for pebbles which are strongly coupled with the gas. In this work, we study the formation of giant planetsincorporating pebble accretion rates in our global model of planet formation.