Mantle differentiation and thermal evolution of Mars, Mercury, and Venus

Details Mantle differentiation and thermal evolution of Mars, Mercury, and Venus Mantle differentiation and thermal evolution of Mars, Mercury, and Venus

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991icar...90..222s&link_type=abstract

Icarus (ISSN 0019-1035), vol. 90, April 1991, p. 222-236. Research supported by DFG and Fullbright Foundation.

Computer Science

73

Mars Surface, Mercury Surface, Planetary Evolution, Planetary Mantles, Planetary Temperature, Venus Surface, Heat Transfer, Lithosphere, Planetary Crusts, Volcanoes, Planets, Mantle, Differentiation, Thermal Properties, Evolution, Mars, Mercury (Planet), Venus, Terrestrial Planets, Core, Chemistry, Crust, Lithosphere, Volcanism, Heat, Thickness, Size, Concentration, Models, Radiogenic Material, Conduction, Thermal History, Calculations, Parameters, Comparisons

Scientific paper

In the present models for the thermal evolution of Mercury, Venus, and Mars encompass core and mantle chemical differentiation, lithospheric growth, and volcanic heat-transfer processes. Calculation results indicate that crust and lithosphere thicknesses are primarily dependent on planet size as well as the bulk concentration of planetary radiogenic elements and the lithosphere's thermal conductivity. The evidence for Martian volcanism for at least 3.5 Gyr, and in Mercury for up to 1 Gyr, in conjunction with the presence of a magnetic field on Mercury and its absence on Mars, suggest the dominance of a lithospheric conduction heat-transfer mechanism in these planets for most of their thermal history; by contrast, volcanic heat piping may have been an important heat-transfer mechanism on Venus.

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