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Title:
Venus - Preliminary prediction of the mineral composition of surface rocks
Authors:
Khodakovskii, I. L.; Volkov, V. P.; Sidorov, Iu. I.; Borisov, M. V.; Lomonosov, M. V.
Affiliation:
AA(Akademiia Nauk SSSR, Institut Geokhimii i Analiticheskoi Khimii, Moscow, USSR), AB(Akademiia Nauk SSSR, Institut Geokhimii i Analiticheskoi Khimii, Moscow, USSR), AC(Akademiia Nauk SSSR, Institut Geokhimii i Analiticheskoi Khimii, Moscow, USSR), AD(Akademiia Nauk SSSR, Institut Geokhimii i Analiticheskoi Khimii, Moscow, USSR), AE(Moskovskii Gosudarstvennyi Universitet, Moscow, USSR)
Publication:
Icarus, vol. 39, Sept. 1979, p. 352-363. (Icarus Homepage)
Publication Date:
09/1979
Category:
Lunar and Planetary Exploration
Origin:
STI
NASA/STI Keywords:
Mineralogy, Petrology, Planetary Composition, Rocks, Venus Surface, Carbon Dioxide Concentration, Carbonization, Geochemistry, Hydration, Iron Oxides, Planetary Evolution, Planetary Temperature, Troposphere, Venus Atmosphere
DOI:
10.1016/0019-1035(79)90146-5
Bibliographic Code:
1979Icar...39..352K

Abstract

A thermodynamical analysis of the multicomponent system Si-Ti-Al-Fe-Mn-Mg-Ca-Na-K-P-C-H-O open with respect to CO2, CO, H2O was carried out. Hydration and carbonization processes are proposed to be geochemical consequences of the hypothesis of quasi-equilibrium conditions between the troposphere and crustal surface rocks. The probable rock-forming hydrated mineral phases are represented by epidote, glaucophane, tremolite, phlogopite, and annite; the carbonatization results in the existence of calcite and dolomite as rock-forming minerals of weathered alkaline lavas. The surface rocks are assumed to have high ferric/ferrous iron ratios. The wollastonite equilibrium is rejected as a buffering chemical reaction. Hydrated minerals could be stable at least up to 5-km depths and contribute about 0.1 x 10 to the 24th g of H2O, whereas about (0.7-0.8) x 10 to the 24th g of H2O would be consumed in ferrous iron oxidation with concomitant hydrogen dissipation. The distribution of H2O in the outer planetary shells is possibly a function of their temperatures.
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