Print Email Facebook Twitter Do tidally-generated inertial waves heat the subsurface oceans of Europa and Enceladus? Title Do tidally-generated inertial waves heat the subsurface oceans of Europa and Enceladus? Author Rovira Navarro, M. (TU Delft Astrodynamics & Space Missions; Universiteit Utrecht; NIOZ Royal Netherlands Institute for Sea Research) Rieutord, Michel (Université de Toulouse; CNRS) Gerkema, Theo (Universiteit Utrecht; NIOZ Royal Netherlands Institute for Sea Research) Maas, Leo R.M. (Universiteit Utrecht) van der Wal, W. (TU Delft Astrodynamics & Space Missions) Vermeersen, L.L.A. (TU Delft Physical and Space Geodesy; TU Delft Astrodynamics & Space Missions; Universiteit Utrecht; NIOZ Royal Netherlands Institute for Sea Research) Date 2019-03-15 Abstract Some of the moons of the outer solar system harbour subsurface liquid oceans. Tidal dissipation plays an important role in preventing these oceans from freezing. In the past, most studies considered only tidal dissipation in the solid layers of these bodies (rock and ice). Recently, new studies considering tidal dissipation in the oceans of these moons have appeared. All of them make use of the shallow water approximation. However, the use of this approximation might not be adequate. Here we consider the linear non-hydrostatic three dimensional response of these oceans to tidal forcing with the full Coriolis force. To do so we consider an ocean of homogeneous density contained within a perfectly spherical shell and neglect the effect of the ice shell. We force the ocean with a time changing tidal potential and observe patterns of periodic inertial waves that take energy from the global tidal forcing and focus it along thin shear layers that propagate in the fluid. We focus on Europa and Enceladus, showing that inertial waves result in fluid flows of significant amplitude (a few cm/s). Nevertheless, we find that under the previously mentioned assumptions tidal dissipation due to inertial waves is several orders of magnitude smaller than Europa's radiogenic heating and Enceladus’ observed heat flux. Finally, we propose additional dissipation mechanisms that might play a relevant role in Europa and Enceladus and could be further investigated. Subject EnceladusEuropaRotational dynamicsTides To reference this document use: http://resolver.tudelft.nl/uuid:73211527-fa02-458b-9adf-3aafb706f145 DOI https://doi.org/10.1016/j.icarus.2018.11.010 Embargo date 2020-11-26 ISSN 0019-1035 Source Icarus, 321, 126-140 Part of collection Institutional Repository Document type journal article Rights © 2019 M. Rovira Navarro, Michel Rieutord, Theo Gerkema, Leo R.M. Maas, W. van der Wal, L.L.A. Vermeersen Files PDF AS69401147185561715424766 ... tent_1.pdf 8.75 MB Close viewer /islandora/object/uuid:73211527-fa02-458b-9adf-3aafb706f145/datastream/OBJ/view