Thermohydrodynamics of Circumstellar Disks with High‐Mass Planets

With a series of numerical simulations, we analyze the thermo-hydrodynamicalevolution of circumstellar disks containing Jupiter-size protoplanets. In theframework of the two-dimensional approximation, we consider an energy equationthat includes viscous heating and radiative effects in a simplified, yetconsistent form. Multiple nested grids are used in order to study both globaland local features around the planet. By means of different viscosityprescriptions, we investigate various temperature regimes. A planetary massrange from 0.1 to 1 Mj is examined. Computations show that gap formation is ageneral property which affects density, pressure, temperature, opticalthickness, and radiated flux distributions. However, it remains a prominentfeature only when the kinematic viscosity is on the order of 10^(15) cm^2/s orlower. Around accreting planets, a circumplanetary disk forms that has asurface density profile decaying exponentially with the distance and whose massis 5-6 orders of magnitudes smaller than Jupiter's mass. Circumplanetary disktemperature profiles decline roughly as the inverse of the distance from theplanet. Temperatures range from some 10 to ~1000 K. Planetary accretion andmigration rates depend on the viscosity regime, with discrepancies within anorder of magnitude. Estimates of growth and migration time scales inferred bythese models are on the same orders of magnitude as those previously obtainedwith locally isothermal simulations.Comment: 31 pages 26 figures. To appear in The Astrophysical Journal vol.599 (December 10, 2003 issue