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    Nonlinear tidal dissipation in the subsurface oceans of Enceladus and other icy satellites

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    HayMatsuyama2018.pdf
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    Author
    Hay, Hamish C.F.C.
    Matsuyama, Isamu cc
    Affiliation
    Univ Arizona, Lunar & Planetary Lab
    Issue Date
    2019-02
    Keywords
    Satellites
    Ocean tides
    Enceladus
    Europa
    Triton
    
    Metadata
    Show full item record
    Publisher
    ACADEMIC PRESS INC ELSEVIER SCIENCE
    Citation
    Hay, H. C., & Matsuyama, I. (2019). Nonlinear tidal dissipation in the subsurface oceans of Enceladus and other icy satellites. Icarus, 319, 68-85.
    Journal
    ICARUS
    Rights
    © 2018 Elsevier Inc. All rights reserved.
    Collection Information
    This 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.
    Abstract
    Subsurface 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.
    Note
    24 month embargo; published online: 18 September 2018
    ISSN
    00191035
    DOI
    10.1016/j.icarus.2018.09.019
    Version
    Final accepted manuscript
    Sponsors
    NASA Earth and Space Science Fellowship (NESSF); NASA [NNX15AQ88G]
    Additional Links
    https://linkinghub.elsevier.com/retrieve/pii/S0019103518304470
    ae974a485f413a2113503eed53cd6c53
    10.1016/j.icarus.2018.09.019
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