Physics
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusm.p22a..04m&link_type=abstract
American Geophysical Union, Spring Meeting 2002, abstract #P22A-04
Physics
5418 Heat Flow, 5430 Interiors (8147), 5480 Volcanism (8450), 8130 Heat Generation And Transport, 8147 Planetary Interiors (5430, 5724)
Scientific paper
Parameterizations of mantle convection have been developed to a high degree of sophistication, incorporating physics such as temperature- and stress-dependent rheology, solid-state phase changes, and continent formation. An important heat transport mechanism that has yet to be investigated systematically is melt segregation and eruption. This process is currently the dominant heat transport mechanism within Jupiter's moon Io, and was undoubtedly important in the early evolution of the terrestrial planets, when large portions of their mantles were super-solidus. The heat flow due to melt segregation depends directly on the internal temperature, which controls the mean depth at which the solidus is crossed, and also on the Rayleigh number which scales the convective velocities in the interior. It is assumed that melt segregation is efficient on timescales much shorter than the convective overturn time. Numerical simulations in the stagnant lid regime of temperature-dependent convection provide estimates for the unknown constants in the relationship between heat flux and internal temperature, which shows a sharp inflection upward at the solidus temperature. The large heat flux due to melt segregation causes rapid cooling of the mantle until the interior temperature reaches the solidus, therefore, unless some large heat source is available such as tidal heating at Io, the period of intense volcanism is correspondingly short.
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