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dc.contributor.authorHay, Hamish C.F.C.
dc.contributor.authorMatsuyama, Isamu
dc.date.accessioned2019-05-16T23:17:34Z
dc.date.available2019-05-16T23:17:34Z
dc.date.issued2019-02
dc.identifier.citationHay, H. C., & Matsuyama, I. (2019). Nonlinear tidal dissipation in the subsurface oceans of Enceladus and other icy satellites. Icarus, 319, 68-85.en_US
dc.identifier.issn00191035
dc.identifier.doi10.1016/j.icarus.2018.09.019
dc.identifier.urihttp://hdl.handle.net/10150/632307
dc.description.abstractSubsurface ocean tides act as a mechanism to dissipate tidal energy in icy satellite interiors. We numerically model the effect of an ice shell on ocean tides using non-linear bottom drag for the first time. We demonstrate that subsurface oceans experience tidal pressurization due to the confining nature of the ice shell, and find that Enceladus' eccentricity forcing can generate up to 2.2 kPa of pressure excess at the ocean surface. Existing free surface oceanic energy dissipation scaling laws are extended to subsurface oceans, and are benchmarked against our numerical results to within 10 %. We show that for the large bodies Ganymede, Europa and Titan, an ice shell increases eccentricity tidal heating due to self-gravity, whereas the shell's suppressive mechanical forcing reduces eccentricity tide dissipation on Enceladus and Dione by several orders of magnitude due to their high effective rigidities. In contrast, the ice shell enhances obliquity-forced dissipation in all satellites investigated, except Triton, because the largely divergence-free ocean response is unaffected by the shell's rigidity but is still enhanced by self-gravity. We conclude that the fundamental difference in ocean response to obliquity and eccentricity forcing, combined with self-gravity, results in increased obliquity heating and suppressed eccentricity heating in small satellites. For large satellites with low effective rigidities, the type of ocean response is less important because the shell's mechanical forcing has little impact on the flow, whereas self-gravity will enhance the response, and consequently dissipation, regardless of the forcing. Overall, obliquity tides are likely to dominate the tidal heating budget of icy satellite oceans, remaining the most prominent source of fluid dissipation in subsurface barotropic ocean tides.en_US
dc.description.sponsorshipNASA Earth and Space Science Fellowship (NESSF); NASA [NNX15AQ88G]en_US
dc.language.isoenen_US
dc.publisherACADEMIC PRESS INC ELSEVIER SCIENCEen_US
dc.relation.urlhttps://linkinghub.elsevier.com/retrieve/pii/S0019103518304470en_US
dc.rights© 2018 Elsevier Inc. All rights reserved.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectSatellitesen_US
dc.subjectOcean tidesen_US
dc.subjectEnceladusen_US
dc.subjectEuropaen_US
dc.subjectTritonen_US
dc.titleNonlinear tidal dissipation in the subsurface oceans of Enceladus and other icy satellitesen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben_US
dc.identifier.journalICARUSen_US
dc.description.note24 month embargo; published online: 18 September 2018en_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal accepted manuscripten_US
dc.source.journaltitleIcarus
dc.source.volume319
dc.source.beginpage68
dc.source.endpage85


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