  Principal regular satellites of gas giants are thought to be formed by the
accumulation of solid materials in circumplanetary disks (CPDs). While there
has been significant progress in the study of satellite formation in CPDs,
details of the supply of satellite building blocks to CPDs remain unclear. We
performed orbital integration of solid particles in the protoplanetary disk
(PPD) approaching a planet, considering the gas drag force using the results of
three-dimensional hydrodynamical simulations of a local region around the
planet. We investigated planetary-mass dependence of the capture positions and
capture rates of dust particles accreting onto the CPD. We also examined the
degree of dust retention in accreting gas onto the CPD, which is important for
determining the ratio of dust-to-gas inflow rates, a key parameter in satellite
formation. We found that the degree of dust retention increases with increasing
planetary mass for a given dust scale height in the PPD. In the case of a small
planet ($M_{\rm p}=0.2M_{\rm Jup}$), most particles with insufficient initial
altitudes in the PPD are isolated from the gas in the accreting region. On the
other hand, in the case of a massive planet ($M_{\rm p}=1M_{\rm Jup}$), dust
particles can be coupled to the vertically accreting gas, even when the dust
scale height is about $10-30$\% of the gas scale height. The results of this
study can be used for models of dust delivery and satellite formation in the
CPDs of gas giants of various masses, including exoplanets.
