Circumplanetary disk ices

The large icy moons of Jupiter formed in a circumplanetary disk (CPD). CPDs are fed by infalling circumstellar gas and dust which may be shock-heated upon accretion or sublimated while passing through an optically thin gap. Accreted material is then either incorporated into moons, falls the planet, lost beyond edge on relatively short timescales. If ices during onto CPD we know there must sufficient time for them to recondense such as Ganymede Callisto could not form. chemical timescale form sufficiently solids places novel constraint dynamical behaviour properties CPDs. We use radiation thermochemical code ProDiMo analyze how radial ice abundance evolves consider different initial conditions explore consequences being inherited from reset atomic shock-heating. contrast timescales formation with those viscous evolution drift. Water can very efficiently initially conditions, significant fraction re-deposited grains within < 1 yr. Radial grain drift general longer than grains. Icy size $a 3$ mm retain their mantles crossing gap at 5 au $L_* 10 $ L$_{\odot}$. Three-body reactions play important role water dense midplane condition depleted relative factor 10-50 produce rock ratio Galilean satellites. snowline erased drift, consistent compositional gradient satellites primordial.