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• W1610361855 startingPage "811" @default.
• W1610361855 abstract "As was the case for Jupiter, Saturn formed either as a result of a gas instability within the solar nebula or the accretion of a solid core that induced an instability within the surrounding solar nebula. In either case, the protoplanet's history can be divided into three major stages: early, quasi-hydrostatic evolution (stage 1); very rapid contraction (stage 2); and late, quasi-hydrostatic contraction (stage 3). During the early history of the Saturn system, giant impact events may have catastrophically disrupted most of the original satellites of Saturn. Such disruption, followed by reaccretion, may be responsible, in part, for the occurrence of Trojans and coorbital moons in the Saturn system, the apparent presence of a stochastic component in the trend of satellite density with radial distance, and the present population of ring particles. Saturn's excess luminosity and viscous dissipation are also discussed in relation to the satellite formation." @default.
• W1610361855 created "2016-06-24" @default.
• W1610361855 creator A5025005070 @default.
• W1610361855 creator A5059238348 @default.
• W1610361855 date "1984-01-01" @default.
• W1610361855 modified "2023-09-26" @default.
• W1610361855 title "Origin and evolution of the Saturn system" @default.
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