Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981icar...47...36c&link_type=abstract
Icarus, vol. 47, July 1981, p. 36-45.
Astronomy and Astrophysics
Astronomy
27
Astronomical Models, Chemical Evolution, Io, Planetary Composition, Planetary Evolution, Planetary Temperature, Free Convection, Galilean Satellites, Iron, Jupiter (Planet), Nebulae, Outgassing, Radioactive Isotopes, Temperature Effects, Data, Composition, Volatile Elements, Oxygen, Fugacity, Carbon Dioxide, Jupiter, Satellites, Io, Models, Thermal Properties, Chemistry, Metals, Evolution, Heating, History, Radionuclides, Tidal Effects, Convection, Outgassing, Water, Methane, Iron Sulfide, Surface, Oxidatio
Scientific paper
A combined thermal and chemical evolution model of Io is presented, outlining limits on the possible starting materials, heating history, chemical history, and present state of Io. Our best scenario starts with Io being accreted from material in a proto-Jovian nebula which condensed between 400-600 K. Radionuclides and tidal heating would lead to large-scale convection within Io and chemical reactions leading to the outgassing of water and methane. Reactions between Fe(0)-FeS and water, at least near the surface, go to completion, resulting in all Fe being oxidized with elemental sulfur producing a low-conductivity crust. In the deep interior, these reactions may not completely exhaust Fe metal, and an FeS-rich core may be formed.
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