Theoretical models of planet formation including planet migration and disk evolution

O. M. GUILERA

Sao Jose do Campos

Congreso; Coloquio Brasilero de Dinámica Orbital; 2018

During last years, observational advances have allowed us to study and characterize exoplanets in different types of planetary systems, as well as to improve our knowledge about the formation and evolution of our Solar System. From a theoretical point of view, it is an important challenge that the models of planetary formation could be able to reproduce the main characteristics of these planetary systems.In this talk I will briefly review our current understanding on how the process of planet formation ocurrs in disks around young stars from the coagulation of micrometer sized dust to the formation of massive gaseous giant planets. After introducing important observational constraints from our own Solar System, extrasolar planetary systems, and from observed protoplanetary disks, I will discuss about the usual initial conditions adopted in planet formation models. Then, I will focus in some of the main physical phenoma invoked in the process of planet formation as protoplanetary disk evolution, drift of pebbles and planetesimals, the accretion of solids by the proto-planets, gas accretion onto massive solid cores, and planet migration. I will emphasize in this last topic, showing that the migration history of a growing planet can be very different respect to previous studies if update type I migration rate prescriptions from new 3D hidrodynamical simulations are adopted (specially those that include the luminosity of the planet due to solid accretion). Finally, I will show that models of planet formation that include these main physical phenomena are able to reproduce the main characteristics of the observed population of extrasolar planets, even the recently observed giant planets in wide orbits.