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The formation of a circumplanetary disk and accretion of angular momentumonto a protoplanetary system are investigated using 3D hydrodynamicalsimulations. The local region around a protoplanet in a protoplanetary disk isconsidered with sufficient spatial resolution: the region from outside the Hillsphere to the Jovian radius is covered by the nested-grid method. Toinvestigate the thermal effects of the circumplanetary disk, various equationsof state are adopted. Large thermal energy around the protoplanet slightlychanges the structure of the circumplanetary disk. Compared with a modeladopting an isothermal equation of state, in a model with an adiabatic equationof state, the protoplanet's gas envelope extends farther, and a slightly thickdisk appears near the protoplanet. However, different equations of state do notaffect the acquisition process of angular momentum for the protoplanetarysystem. Thus, the specific angular momentum acquired by the system is fitted asa function only of the protoplanet's mass. A large fraction of the totalangular momentum contributes to the formation of the circumplanetary disk. Thedisk forms only in a compact region in very close proximity to the protoplanet.Adapting the results to the solar system, the proto-Jupiter and Saturn havecompact disks in the region of r < 21 r_J (r < 0.028 r_HJ) and r < 66 r_S (r <0.061 r_HS), respectively, where r_J (r_HJ) and r_S (r_HS) are the Jovian andSaturnian (Hill) radius, respectively. The surface density has a peak in theseregions due to the balance between centrifugal force and gravity of theprotoplanet. The size of these disks corresponds well to the outermost orbit ofregular satellites around Jupiter and Saturn. Regular satellites may form insuch compact disks around proto-gas giant planets.

Thermal Effects of Circumplanetary Disk Formation around Proto-Gas Giant Planets