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As the number of discovered extrasolar planets has been increasing, diversityof planetary systems requires studies of new formation scenarios. It isimportant to study satellite formation in circumplanetary disks, which is oftenviewed as analogous to formation of rocky planets in protoplanetary disks. Weinvestigated satellite formation from satellitesimals around giant planetsthrough N-body simulations that include gravitational interactions with acircumplanetary gas disk. Our main aim is to reproduce the observableproperties of the Galilean satellites around Jupiter through numericalsimulations, as previous N-body simulations have not explained the origin ofthe resonant configuration. We performed accretion simulations based on thework of Sasaki et al. (2010), in which an inner cavity is added to the model ofCanup & Ward (2002, 2006). We found that several satellites are formed andcaptured in mutual mean motion resonances outside the disk inner edge and arestable after rapid disk gas dissipation, which explains the characteristics ofthe Galilean satellites. In addition, owing to the existence of the disk edge,a radial compositional gradient of the Galilean satellites can also bereproduced. An additional objective of this study is to discuss orbitalproperties of formed satellites for a wide range of conditions by consideringlarge uncertainties in model parameters. Through numerical experiments andsemianalytical arguments, we determined that if the inner edge of a disk isintroduced, a Galilean-like configuration in which several satellites arecaptured into a 2:1 resonance outside the disk inner cavity is almostuniversal. In fact, such a configuration is produced even for a massive diskand rapid type I migration. This result implies the inevitability of a Galileansatellite formation in addition to providing theoretical predictions forextrasolar satellites.

N-body Simulations of Satellite Formation around Giant Planets: Origin of Orbital Configuration of the Galilean Moons