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The four major satellites of Jupiter, known as the Galilean moons, andSaturn's most massive satellite, Titan, are believed to have formed in apredominantly gaseous circum-planetary disk, during the last stages offormation of their parent planet. Pebbles from the protoplanetary disk areblocked from flowing into the circumplanetary disk by the positive pressuregradient at the outer edge of the planetary gap, so the gas drag assistedcapture of planetesimals should be the main contributor to the delivery ofsolids onto circum-planetary disks. However, a consistent framework for thesubsequent accretion of the moons remains to be built. Here we use numericalintegrations to show that most planetesimals being captured within acircum-planetary disk are strongly ablated due to the frictional heating theyexperience, thus supplying the disk with small dust grains, whereas only asmall fraction 'survives' their capture. We then construct a simple model of acircum-planetary disk supplied by ablation, where the flux of solids throughthe disk is at equilibrium with the ablation supply rate, and investigate theformation of moons in such disks. We show that the growth of satellites isdriven mainly by accretion of the pebbles that coagulate from the ablatedmaterial. The pebble-accreting protosatellites rapidly migrate inward and pileup in resonant chains at the inner edge of the circum-planetary disk. Wepropose that dynamical instabilities in these resonant chains are at the originof the different architectures of Jupiter's and Saturn's moon systems. Theassembly of moon systems through pebble accretion can therefore be seen as adown-scaled manifestation of the same process that forms systems ofsuper-Earths and terrestrial-mass planets around solar-type stars and M-dwarfs.

Formation of moon systems around giant planets: Capture and ablation of planetesimals as foundation for a pebble accretion scenario