We find that moderately high orbital eccentricities can be obtained, but show that the nonhydrostatic shape of the Moon cannot be explained by the shape solution of Garrick-Bethell et al. We compute the tidal heating in a dissipative lid overlying a magma ocean and the associated tidal evolution of the lunar orbit. Next, we create a coupled thermal-orbital model for the early evolution of the Moon. We conclude that the most likely explanation for Enceladus' anomalous heat flow is a QS lower than 18,000, which implies either time or frequency dependent dissipation for Saturn. ![]() We find that Enceladus does not experience oscillations in heat flow for any choice of parameters. We also look for thermal disequilibrium using the oscillation model of Ojakangas and Stevenson (1986). We find that Enceladus is at or near equilibrium in its current 2:1 mean motion resonance with Dione. We then look for dynamical disequilibrium by constructing a resonance model, tested by n-body integrations, to establish a consistent resonance history for Mimas, Enceladus, and Dione. The constraint on the heat flow is calculated from simple conservation of energy and angular momentum arguments and does not depend on the internal parameters of the satellites. We constrain the equilibrium heating of Enceladus to be less than 1.1(18000/QS) GW, where QS is the tidal quality factor of Saturn. First, we study the effects of tidal heating and tidal evolution in the Saturnian satellite system. ![]() In this thesis, we examine the effects of tidal dissipation on solid bodies in application and in theory.
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