Venus - Preliminary prediction of the mineral composition of surface rocks

Details Venus - Preliminary prediction of the mineral composition of surface rocks Venus - Preliminary prediction of the mineral composition of surface rocks

Sep 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979icar...39..352k&link_type=abstract

Icarus, vol. 39, Sept. 1979, p. 352-363.

Computer Science

4

Mineralogy, Petrology, Planetary Composition, Rocks, Venus Surface, Carbon Dioxide Concentration, Carbonization, Geochemistry, Hydration, Iron Oxides, Planetary Evolution, Planetary Temperature, Troposphere, Venus Atmosphere

Scientific paper

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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