Physics
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufm.p12a0491m&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #P12A-0491
Physics
5418 Heat Flow, 5430 Interiors (8147), 5480 Volcanism (8450), 8147 Planetary Interiors (5430, 5724), 8450 Planetary Volcanism (5480)
Scientific paper
Silicate volcanism is well established at Io, adding to the curiosity of Jupiter's innermost large satellite. It is clear that a balance between tidal heating and convective heat transport in Io results in a stable equilibrium with internal temperatures are somewhat above the solidus, because dissipation is still increasing as the solidus is crossed. As the rocks of Io's mantle begin to melt, an interconnected network of melt forms, allowing the less dense melt to percolate upwards. In steady state, this melt is replaced by a slower flow of solid downward. The net result of this segregation is the transport of latent heat with the melt, which eventually is deposited at the surface. Quantitative solution of the equations of melt transport coupled to tidal heating rates derived from a layered, Maxwell-viscoelastic model of Io reveal that the heat transported by melt segregation overwhelms (and shuts down) convective heat transport in Io's mantle when melt fractions exceed a few percent. This leads to a new heat balance in Io, which predicts maximum melt fractions less than 20%, and interior temperatures near the solidus. Since the solidus temperature increases with pressure, the deep mantle is probably convecting. Combining parameterized convection models with melt segregation heat transport and a parameterization of heat-pipe transport in the lithosphere allows the calculation of Io's internal temperatures consistent with the surface heat flow.
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