Physics
Scientific paper
Jan 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000pepi..117..407z&link_type=abstract
Physics of the Earth and Planetary Interiors, Volume 117, Issue 1-4, p. 407-420.
Physics
11
Scientific paper
A set of global interior structure models for Mars, which agree with the Mars Pathfinder (MPF) value of the mean moment of inertia factor is constructed. The models are obtained by combining the crust models of Babeiko and Zharkov [Babeiko, A.Yu., Zharkov, V.N., 1997. Mineralogical composition and seismic model of the Martian crust. Sol. Syst. Res. 31, 361-368 Babeiko, A.Yu., Zharkov, V.N., 1998. Density and seismic profiles of the Martian crust in the event of an extra-low temperature gradient. Sol. Syst. Res. 32, 14-16] with the model Martian mantle of Bertka and Fei [Bertka, C.M., Fei, Y., 1996. A profile of Martian mantle mineralogy and density up to core-mantle boundary pressures. Lunar Planet. Sci. XXVII, 107-108 Bertka, C.M., Fei, Y., 1997. Mineralogy of the Martian interior up to core-mantle boundary pressures. J. Geophys. Res. 102, 5251-5264.] and the core model of Zharkov [Zharkov, V.N., 1996. The internal structure of Mars: a key to understanding the origin of terrestrial planets. Sol. Syst. Res. 30, 456-465]. The models of the crust are constructed by numerical thermodynamic simulation by using the compositions of basaltic SNC meteorites. The model Martian mantle is based on mineral physics data obtained by recent high pressure experiments. These laboratory measurements were carried out by Bertka and Fei (1997) along a model marstherm up to core pressures of Mars using mineral mixtures with the cosmochemical composition proposed by Dreibus and Wänke [Dreibus, G., Wänke, H., 1989. Supply and loss of volatile constituents during the accretion of terrestrial planets. In: Atreya, S.K., Pollack, J.B., Matthews, M.S. (Eds.), Origin and Evolution of Planetary and Satellite Atmospheres. Univ. Arizona Press, pp. 268-288.] and Wänke and Dreibus [Wänke, H., Dreibus, G., 1994. Chemistry and accretion history of Mars. Philos. Trans. R. Soc. London 349, 285-293.] (DW composition). The model of the core is also constructed for this composition, but the fact that the Martian core may contain a significant amount of hydrogen is taken into account. Based on an analogy with Earth, where the iron content in crust basalts is noticeably higher than in mantle silicates, we have calculated a set of models with a molecular concentration of iron in the Martian mantle equal to 20 mol%, rather than 25 mol% (DW composition). For models with this modified iron content of the mantle and the values of hydrogen content in the core between 0 and 50 mol%, the Fe/Si weight ratio is found to vary from 1.525 to 1.695. This is in good accord with the chondritic value of 1.71, predicted by Dreibus and Wänke's chemical model of Mars. Only a determination of the planetary core radius with sufficiently high accuracy can substantially improve our understanding of the Martian interior. The parameters of the equilibrium figure of Mars are calculated for the constructed models.
Gudkova T. V.
Zharkov Vladimir Naumovich
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