  Saturn has a dynamically rich satellite system, which includes at least three
orbital resonances between three pairs of moons: Mimas-Tethys 4:2,
Enceladus-Dione 2:1, and Titan-Hyperion 4:3 mean-motion resonances. Studies of
the orbital history of Saturn's moons usually assume that their past dynamics
was also dominated solely by two-body resonances. Using direct numerical
integrations, we find that three-body resonances among Saturnian satellites
were quite common in the past, and could result in a relatively long-term, but
finite capture time (10 Myr or longer). We find that these three-body
resonances are invariably of the eccentricity type, and do not appear to affect
the moons' inclinations. While some three-body resonances are located close to
two-body resonances (but involve the orbital precession of the third body),
others are isolated, with no two-body arguments being near resonance. We
conclude that future studies of the system's past must take full account of
three-body resonances, which have been overlooked in the past work.
