  We report on the results of novel global high-resolution three-dimensional
simulations of disk-planet interaction which incorporate simultaneously
realistic radiation physics and the self-gravity of the gas, as well as
allowing the planet to move. We find that thermodynamics and radiative physics
have a remarkable effect on both migration and accretion of Jupiter mass
planets. In simulations with radiative transfer adopting flux-limited
diffusion, inward migration can be decreased by about 30% relative to the
isothermal case, while in adiabatic runs migration nearly shuts off after a few
tens of orbits. Migration varies because the relative strength of the inner and
outer spiral perturbations is affected by thermodynamics, thus changing the net
torque acting on the planet. Mass accretion rates on the planet can be reduced
by more than an order of magnitude going from isothermal to radiative transfer
and adiabatic simulations. A circumplanetary disk always forms except in
adiabatic runs. With radiative transfer the disk is sub-keplerian (Vrot/Vkep ~
0.7) owing to significant pressure support. We discuss the effect of
circumplanetary disk structure on the drift of embedded dust grains and
planetesimals and thus on the formation of the rocky satellites of giant
planets.
