We study the evolution of planetesimals in evolved gaseous disks , which orbit a solar-mass star and harbor a Jupiter-mass planet at a _ { p } \approx 5 \mbox { AU } .
The gas dynamics is modeled with a three-dimensional hydrodynamics code that employes nested-grids and achieves a resolution of one Jupiter ’ s radius in the circumplanetary 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 through ablation .
The mass evolution of solids is calculated self-consistently with their temperature , velocity , and position .
We consider icy and icy/rocky bodies of radius 0.1 – 100 \mathrm { km } , initially deployed on orbits around the star within a few Hill radii ( R _ { \mathrm { H } } ) of the planet ’ s orbit .
Planetesimals are scattered inward , outward , and toward disk regions of radius r \gg a _ { p } .
Scattering can relocate significant amounts of solids , provided that regions |r - a _ { p } | \sim 3 \mbox { $R _ { \mathrm { H } } $ } are replenished with planetesimals .
Scattered bodies can be temporarily captured on planetocentric orbits .
Ablation consumes nearly all solids at gas temperatures \gtrsim 220 \mbox { $ \mathrm { K } $ } .
Super-keplerian rotation around and beyond the outer edge of the gas gap can segregate \lesssim 0.1 \mathrm { km } bodies , producing solid gap edges at size-dependent radial locations .
Capture , break-up , and ablation of solids result in a dust-laden circumplanetary disk with low surface densities of \mathrm { km } -size planetesimals , implying relatively long timescales for satellite formation .
After a giant planet acquires most of its mass , accretion of solids is unlikely to alter significantly its heavy-element content .
The luminosity generated by solids ’ accretion can be of a similar order of magnitude to the contraction luminosity .