Internal energy dissipation in Enceladus's ocean from tides and libration and the role of inertial waves

Abstract

Enceladus is characterised by a south polar hot spot associated with a large outflow of heat, the source of which remains unclear. We compute the viscous dissipation resulting from tidal and libration forcing in the moon's subsurface ocean using the linearised Navier-Stokes equation in a 3-dimensional spherical model. We conclude that libration is the dominant cause of dissipation at the linear order, providing up to about 0.001 GW of heat to the ocean, which remains insufficient to explain the (about) 10 GW observed by Cassini. We also illustrate how resonances with inertial modes can significantly augment the dissipation. Our work is an extension to Rovira-Navarro et al. [2019] to include the effects of libration. The model developed here is readily applicable to the study of other moons and planets.

References in corpus (12)

• Enceladus's measured physical libration requires a global subsurface ocean
• Geophysical tests for habitability in ice-covered ocean worlds
• Inertial waves in a rotating spherical shell: attractors and asymptotic spectrum
• Tides in rotating barotropic fluid bodies: the contribution of inertial waves and the role of internal structure
• Enceladus's and Dione's floating ice shells supported by minimum stress isostasy
• Tidal dissipation in rotating fluid bodies: a simplified model
• Ocean tidal heating in icy satellites with solid shells
• Tidal dissipation in rotating fluid bodies: the presence of a magnetic field
• The obliquity of Enceladus
• Completeness of Inertial Modes of an Incompressible Non-Viscous Fluid in a Corotating Ellipsoid
• The coupling between inertial and rotational eigenmodes in planets with liquid cores
• Inertial Modes in Near-Spherical Geometries

Cited by in corpus (10)

• Ocean Circulation on Enceladus With a High Versus Low Salinity Ocean
• Powering the Galilean Satellites with Moon-Moon Tides
• Different ice shell geometries on Europa and Enceladus due to their different sizes: impacts of ocean heat transport
• Resonant tidal responses in rotating fluid bodies: global modes hidden beneath localized wave beams
• Probing the icy shell structure of ocean worlds with gravity-topography admittance
• The role of ocean circulation in driving hemispheric symmetry breaking of the ice shell of Enceladus
• The effect of salinity on ocean circulation and ice-ocean interaction on Enceladus
• Tidal synchronization trapping in stars and planets with convective envelopes
• Anisotropic tidal dissipation in misaligned planetary systems
• New constraint on Europa's ice shell: magnetic signature from the ocean