Tidal heating and convection in Io

Details Tidal heating and convection in Io Tidal heating and convection in Io

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003jgre..108.5096m&link_type=abstract

Journal of Geophysical Research, Volume 108, Issue E8, pp. 15-1, CiteID 5096, DOI 10.1029/2002JE001943

Physics

17

Planetary Sciences: Heat Flow, Planetary Sciences: Interiors (8147), Planetary Sciences: Volcanism (8450), Planetology: Solar System Objects: Jovian Satellites, Tectonophysics: Dynamics, Convection Currents And Mantle Plumes

Scientific paper

The prodigious heat flux emitted from the surface of Jupiter's moon Io is produced in the interior of the satellite by viscoelastic dissipation of tidal energy and is generally thought to be brought to the surface by convective motions. New models of Io's equilibrium thermal state are constructed using self-consistent calculations of tidal heating and convective heat transport. These models show that while a high-temperature convective equilibrium exists, it falls an order of magnitude short of explaining the observed heat flux. Either Io is currently out of thermal equilibrium, or another heat transport mechanism such as melt segregation determines Io's thermal state.

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