  Gas accretion onto the circumplanetary disks and the source region of
accreting gas are important to reveal dust accretion that leads to satellite
formation around giant planets. We performed local three-dimensional
high-resolution hydrodynamic simulations of isothermal and inviscid gas flow
around a planet to investigate planetary-mass dependence of gas accretion band
width and gas accretion rate onto circumplanetary disks. We examined cases with
various planetary masses corresponding to M_p=0.05-1M_{Jup} at 5.2 au, where
M_{Jup} is the current Jovian mass. We found that the radial width of the gas
accretion band is proportional to M_p^{1/6} for the low-mass regime with M_p <
0.2 M_{Jup} while it is proportional to M_p for the high-mass regime with M_p >
0.2M_{Jup}. We found that the ratio of the mass accretion rate onto the
circumplanetary disk to that into the Hill sphere is about 0.4 regardless of
planetary mass for the cases we examined. Combining our results with the gap
model obtained from global hydrodynamic simulations, we derive semi-analytical
formulae of mass accretion rate onto circumplanetary disks. We found that the
mass dependence of our three-dimensional accretion rates is the same as the
previously-obtained two-dimensional case, although the qualitative behavior of
accretion flow onto the CPD is quite different between the two cases.
