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We report on the results of novel global high-resolution three-dimensionalsimulations of disk-planet interaction which incorporate simultaneouslyrealistic radiation physics and the self-gravity of the gas, as well asallowing the planet to move. We find that thermodynamics and radiative physicshave a remarkable effect on both migration and accretion of Jupiter massplanets. In simulations with radiative transfer adopting flux-limiteddiffusion, inward migration can be decreased by about 30% relative to theisothermal case, while in adiabatic runs migration nearly shuts off after a fewtens of orbits. Migration varies because the relative strength of the inner andouter spiral perturbations is affected by thermodynamics, thus changing the nettorque acting on the planet. Mass accretion rates on the planet can be reducedby more than an order of magnitude going from isothermal to radiative transferand adiabatic simulations. A circumplanetary disk always forms except inadiabatic runs. With radiative transfer the disk is sub-keplerian (Vrot/Vkep ~0.7) owing to significant pressure support. We discuss the effect ofcircumplanetary disk structure on the drift of embedded dust grains andplanetesimals and thus on the formation of the rocky satellites of giantplanets.

Migration and growth of giant planets in self-gravitating disks with varied thermodynamics