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Saturn's mid-sized moons (satellites) have a puzzling orbital configurationwith trapping in mean-motion resonances with every other pairs (Mimas-Tethys4:2 and Enceladus-Dione 2:1). To reproduce their current orbital configurationon the basis of Crida & Charnoz's model of satellite formation from ahypothetical ancient massive rings, adjacent pairs must pass 1st-ordermean-motion resonances without being trapped. The trapping could be avoided byfast orbital migration and/or excitation of the satellite's eccentricity causedby gravitational interactions between the satellites and the rings (the disk),which are still unknown. In our research, we investigate the satellite orbitalevolution due to interactions with the disk through full N-body simulations. Weperformed global high-resolution N-body simulations of a self-gravitatingparticle disk interacting with a single satellite. We used $N \sim 10^5$particles for the disk. Gravitational forces of all the particles and theirinelastic collisions are taken into account. As a result, denseshort-wavelength wake structure is created by the disk self-gravity and globalspiral arms with $m \sim$ a few is induced by the satellite. The self-gravitywakes regulate the orbital evolution of the satellite, which has beenconsidered as a disk spreading mechanism but not as a driver for the orbitalevolution. The self-gravity wake torque to the satellite is so effective thatthe satellite migration is much faster than that was predicted with the spiralarms torque. It provides a possible model to avoid the resonance capture ofadjacent satellite pairs and establish the current orbital configuration ofSaturn's mid-sized satellites.

Orbital evolution of Saturn's satellites due to the interaction between the moons and massive Saturn's rings