Ocean tidal heating in icy satellites with solid shells

Isamu M Matsuyama, Mikael Beuthe, Hamish C.F.C. Hay, Francis Nimmo, Shunichi Kamata

Research output: Contribution to journalArticle

8 Citations (Scopus)

Abstract

As a long-term energy source, tidal heating in subsurface oceans of icy satellites can influence their thermal, rotational, and orbital evolution, and the sustainability of oceans. We present a new theoretical treatment for tidal heating in thin subsurface oceans with overlying incompressible elastic shells of arbitrary thickness. The stabilizing effect of an overlying shell damps ocean tides, reducing tidal heating. This effect is more pronounced on Enceladus than on Europa because the effective rigidity on a small body like Enceladus is larger. For the range of likely shell and ocean thicknesses of Enceladus and Europa, the thin shell approximation of Beuthe (2016) is generally accurate to less than about 4%. Explaining Enceladus’ endogenic power radiated from the south polar terrain by ocean tidal heating requires ocean and shell thicknesses that are significantly smaller than the values inferred from gravity and topography constraints. The time-averaged surface distribution of ocean tidal heating is distinct from that due to dissipation in the solid shell, with higher dissipation near the equator and poles for eccentricity and obliquity forcing, respectively. This can lead to unique horizontal shell thickness variations if the shell is conductive. The surface displacement driven by eccentricity and obliquity forcing can have a phase lag relative to the forcing tidal potential due to the delayed ocean response. For Europa and Enceladus, eccentricity forcing generally produces greater tidal amplitudes due to the large eccentricity values relative to the obliquity values. Despite the small obliquity values, obliquity forcing generally produces larger phase lags due to the generation of Rossby–Haurwitz waves. If Europa's shell and ocean are, respectively, 10 and 100 km thick, the tide amplitude and phase lag are 26.5 m and <1° for eccentricity forcing, and <2.5 m and <18° for obliquity forcing. Measurement of the obliquity phase lag (e.g. by Europa Clipper) would provide a probe of ocean thickness

Original languageEnglish (US)
Pages (from-to)208-230
Number of pages23
JournalIcarus
Volume312
DOIs
StatePublished - Sep 15 2018

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icy satellites
oceans
obliquity
shell
heating
Enceladus
Europa
ocean
eccentricity
time lag
tides
dissipation
ocean tide
elastic shells
rigidity
energy sources
equators
tide
topography
probe

Keywords

  • Dynamics
  • Enceladus
  • Europa
  • Rotational dynamics
  • Satellites
  • Solid body
  • Tides

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Matsuyama, I. M., Beuthe, M., Hay, H. C. F. C., Nimmo, F., & Kamata, S. (2018). Ocean tidal heating in icy satellites with solid shells. Icarus, 312, 208-230. https://doi.org/10.1016/j.icarus.2018.04.013

Ocean tidal heating in icy satellites with solid shells. / Matsuyama, Isamu M; Beuthe, Mikael; Hay, Hamish C.F.C.; Nimmo, Francis; Kamata, Shunichi.

In: Icarus, Vol. 312, 15.09.2018, p. 208-230.

Research output: Contribution to journalArticle

Matsuyama, IM, Beuthe, M, Hay, HCFC, Nimmo, F & Kamata, S 2018, 'Ocean tidal heating in icy satellites with solid shells', Icarus, vol. 312, pp. 208-230. https://doi.org/10.1016/j.icarus.2018.04.013
Matsuyama, Isamu M ; Beuthe, Mikael ; Hay, Hamish C.F.C. ; Nimmo, Francis ; Kamata, Shunichi. / Ocean tidal heating in icy satellites with solid shells. In: Icarus. 2018 ; Vol. 312. pp. 208-230.
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