Giant Planet Formation

Our group is engaged in the modelling of gas giant planet formation, in the framework of the core-accretion scenario. These models take into account the migration of the forming planet, and the evolution of the protoplanetary disk, as a result of viscosity and photo-evaporation. The models allow the formation of giant planets in a time well within the observed lifetime of protoplanetary disks and are able to explain the internal structure and atmospheric composition of Jupiter and Saturn.