Magnetism and thermal evolution of the terrestrial planets

Details Magnetism and thermal evolution of the terrestrial planets Magnetism and thermal evolution of the terrestrial planets

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983icar...54..466s&link_type=abstract

Icarus (ISSN 0019-1035), vol. 54, June 1983, p. 466-489. Research supported by the Deutsche Forschungsgemeinschaft.

Astronomy and Astrophysics

Astronomy

304

Planetary Cores, Planetary Evolution, Planetary Magnetic Fields, Planetary Temperature, Terrestrial Planets, Astronomical Models, Cooling, Dynamo Theory, Free Convection, Parameterization, Thermal Energy, Planets, Terrestrial Planets, Magnetism, Thermal Effects, Evolution, Magnetic Properties, Magnetic Fields, Cores, Dynamos, Thermal History, Earth, Mercury(Planet), Venus, Mars, Models, Comparsions, Mantles, Convection, Heating, Cooling, Physical Properties, Parameters

Scientific paper

Of the terrestrial planets, Earth and probably Mercury possess substantial intrinsic magnetic fields generated by core dynamos, while Venus and Mars apparently lack such fields. Thermal histories are calculated for these planets and are found to admit several possible present states, including those which suggest simple explanations for the observations. All of the models presented assume that (1) core dynamos are driven by thermal and/or chemical convection; (2) radiogenic heat production is confined to the mantle; (3) mantle and core cool from initially hot states which are at the solidus and superliquidus, respectively; and (4) any inner core excludes the light alloying material (sulfur or oxygen) which then mixes uniformly upward through the outer core. The models include realistic pressure and composition-dependent freezing curves for the core, and material parameters are chosen so that the correct present-day values of heat outflow, upper mantle temperature and viscosity, and inner core radius are obtained for the Earth.

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