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We study the evolution of planetesimals in evolved gaseous disks, which orbita solar-mass star and harbor a Jupiter-mass planet at a_p~5AU. The gas dynamicsis modeled with a three-dimensional hydrodynamics code that employesnested-grids and achieves a resolution of one Jupiter's radius in thecircumplanetary disk. The code models solids as individual particles.Planetesimals are subjected to gravitational forces by the star and the planet,drag force by the gas, disruption via ram pressure, and mass loss throughablation. The mass evolution of solids is calculated self-consistently withtheir temperature, velocity, and position. We consider icy and icy/rocky bodiesof radius 0.1-100km, initially deployed on orbits around the star within a fewHill radii (Rhill) of the planet's orbit. Planetesimals are scattered inward,outward, and toward disk regions of radius r>>a_p. Scattering can relocatesignificant amounts of solids, provided that regions |r-a_p|~ 3Rhill arereplenished with planetesimals. Scattered bodies can be temporarily captured onplanetocentric orbits. Ablation consumes nearly all solids at gas temperatures> ~220K. Super-keplerian rotation around and beyond the outer edge of the gasgap can segregate < ~0.1km bodies, producing solid gap edges at size-dependentradial locations. Capture, break-up, and ablation of solids result in adust-laden circumplanetary disk with low surface densities of km-sizeplanetesimals, implying relatively long timescales for satellite formation.After a giant planet acquires most of its mass, accretion of solids is unlikelyto alter significantly its heavy-element content. The luminosity generated bysolids' accretion can be of a similar order of magnitude to the contractionluminosity.

Capture and Evolution of Planetesimals in Circumjovian Disks