Tidal viscosity of Enceladus

Abstract

In the preceding paper (Efroimsky 2017), we derived an expression for the tidal dissipation rate in a homogeneous near-spherical Maxwell body librating in longitude. Now, by equating this expression to the outgoing energy flux due to the vapour plumes, we estimate the mean tidal viscosity of Enceladus, under the assumption that the Enceladean mantle behaviour is Maxwell. This method yields a value of $\,0.24\times 10^{14}\;\mbox{Pa~s}\,$ for the mean tidal viscosity, which is very close to the viscosity of ice near the melting point.

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• Orbital relaxation and excitation of planets tidally interacting with white dwarfs
• Tidal synchronization of close-in satellites and exoplanets. III. Tidal dissipation revisited and application to Enceladus
• Dissipation in a tidally perturbed body librating in longitude
• Rotation and figure evolution in the creep tide theory. A new approach and application to Mercury
• Exploring the Interior Structure and Mode of Tidal Heating in Enceladus
• A Simplified Model for the Forced Libration of Icy Moons with Subsurface Oceans: Application to Enceladus and Mimas
• Creep tide theory. Equations for differentiated bodies with aligned layers