  Circumplanetary disks regulate the late accretion to the giant planet and
serve as the birthplace for satellites. Understanding their characteristics via
simulations also helps to prepare for their observations. Here we study disks
around 1, 3, 5, 10 $\mathrm{M_{Jup}}$ planets with three dimensional, global
radiative hydrodynamic simulations with sub-planet peak resolution, and various
planetary temperatures. We found that as the 1 $\mathrm{M_{Jup}}$ planet
radiates away its formation heat, the circumplanetary envelope transitions to a
disk between $T_p = 6000$ K and 4000 K. In the case of 3-10 $\mathrm{M_{Jup}}$
planets a disk always forms. The temperature profile of the circumplanetary
disks is very steep, the inner 1/6th is over the silicate condensation
temperature and the entire disk is above water freezing point, making satellite
formation impossible in this early stage ($<$1 Myr). Satellites might form much
later and first in the outer parts of the disk migrating inwards later on. Our
disk masses are $1, 7, 20, 40 \times 10^{-3}\mathrm{M_{Jup}}$ for the 1, 3, 5,
10 $\mathrm{M_{Jup}}$ gas giants respectively, and we provide an empirical
formula to estimate the subdisk masses based on the planet- and circumstellar
disk mass. Our finding is that the cooler the planet, the lower the temperature
of the subdisk, the higher the vertical influx velocities, and the planetary
gap is both deeper and wider. We also show that the gaps in 2D and 3D are
different. The subdisk eccentricity increases with planetary mass and violently
interacts with the circumstellar disk, making satellite-formation less likely,
if $\mathrm{M_p} \gtrsim 5 \mathrm{M_{Jup}}$.
