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Regular satellites of giant planets are formed by accretion of solid bodiesin circumplanetary disks. Planetesimals that are moving on heliocentric orbitsand are sufficiently large to be decoupled from the flow of the protoplanetarygas disk can be captured by gas drag from the circumplanetary disk. In thepresent work, we examine the distribution of captured planetesimals incircumplanetary disks using orbital integrations. We find that the number ofcaptured planetesimals reaches an equilibrium state as a balance betweencontinuous capture and orbital decay into the planet. The number ofplanetesimals captured into retrograde orbits is much smaller than those onprograde orbits, because the former ones experience strong headwind and spiralinto the planet rapidly. We find that the surface number density ofplanetesimals at the current radial location of regular satellites can besignificantly enhanced by gas drag capture, depending on the velocitydispersions of planetesimals and the width of the gap in the protoplanetarydisk. Using a simple model, we also examine the ratio of the surface densitiesof dust and captured planetesimals in the circumplanetary disk, and find thatsolid material at the current location of regular satellites can be dominatedby captured planetesimals when the velocity dispersion of planetesimals israther small and a wide gap is not formed in the protoplanetary disk. In thiscase, captured planetesimals in such a region can grow by mutual collisionbefore spiraling into the planet, and would contribute to the growth of regularsatellites.

Distribution of captured planetesimals in circumplanetary gas disks and implications for accretion of regular satellites