Physics
Scientific paper
Mar 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987em%26p...37..287f&link_type=abstract
Earth, Moon, and Planets (ISSN 0167-9295), vol. 37, March 1987, p. 287-313.
Physics
11
Hydrogeology, Mars (Planet), Planetary Evolution, Planetary Temperature, Planetology, Planetary Cores, Planetary Magnetic Fields, Planetary Mantles, Silicates, Solidus, Thermal Boundary Layer
Scientific paper
Conventional evolutionary models for Mars adopt a dry mantle solidus. Taking into account the condensation conditions in the preplanetary nebula in the accretion zone of Mars, it can be concluded that large amounts of water or hydrated silicates have condensed in those regions. Therefore, water influences significantly the melting behaviour and the viscosity of the silicatic material. A model for the calculation of the thermal history of a planet is constructed. On this basis, and use of water - saturated solidus - it is possible to derive that the core is not liquid, as given in models employing a dry mantle solidus, but solid to a large extent, which prevents the operation of a large-scale dynamo and explains in that way the lack of a magnetic field. With these assumptions one can construct a possible evolutionary scheme that covers early crust differentiation, a hot thermal past and the missing magnetic field at present.
Franck Siegfried
Orgzall Ingo
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