Abstract
We utilize Earth-based, Earth-orbital, and spacecraft observations
of the atmosphere and surface of Venus, thermodynamic models of atmosphere-lithosphere
interactions, and where available kinetic data on relevant gas-solid
reactions to place constraints on the mineralogy of the surface of
Venus. We discuss which minerals and mineral assemblages are stable
on the surface of Venus and which, if any, of these minerals are
involved in controlling the abundances of reactive gases in the atmosphere
of Venus. We conclude by identifying key issues facing us today about
the mineralogy and geochemistry of the surface of Venus and suggest
experimental, observational, and theoretical studies that can improve
our knowledge of these important questions.
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