  With a series of numerical simulations, we analyze the thermo-hydrodynamical
evolution of circumstellar disks containing Jupiter-size protoplanets. In the
framework of the two-dimensional approximation, we consider an energy equation
that includes viscous heating and radiative effects in a simplified, yet
consistent form. Multiple nested grids are used in order to study both global
and local features around the planet. By means of different viscosity
prescriptions, we investigate various temperature regimes. A planetary mass
range from 0.1 to 1 Mj is examined. Computations show that gap formation is a
general property which affects density, pressure, temperature, optical
thickness, and radiated flux distributions. However, it remains a prominent
feature only when the kinematic viscosity is on the order of 10^(15) cm^2/s or
lower. Around accreting planets, a circumplanetary disk forms that has a
surface density profile decaying exponentially with the distance and whose mass
is 5-6 orders of magnitudes smaller than Jupiter's mass. Circumplanetary disk
temperature profiles decline roughly as the inverse of the distance from the
planet. Temperatures range from some 10 to ~1000 K. Planetary accretion and
migration rates depend on the viscosity regime, with discrepancies within an
order of magnitude. Estimates of growth and migration time scales inferred by
these models are on the same orders of magnitude as those previously obtained
with locally isothermal simulations.
