Introduction to Venus Surface
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This study presents an inventory of possible chemical reactions affecting, or having affected, the Venus surface.
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We also present the dielectric constant ({\epsilon}) values of the Venus surface estimated using the degree of polarisation maps of Venus, derived from the GMRT polarisation observations and theoretical calculations.
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The infrared radiative flux to the Venus surface due to \(\mathrm{CO}_2\) is about 30% of the total flux, and the other part is determined by a dust.
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Identifying such silica‐rich flows on Venus would imply that the composition of the Venus surface and interior is Earth‐like and possibly water‐rich.
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Prolonged Venus surface missions (lasting months instead of hours) have proven infeasible to date in the absence of a complete suite of electronics able to function for such durations without protection from the planet’s extreme conditions of ~460°C, ~9.
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First global map of Venus nightside surface temperature using Akatsuki infrared measurements reveals hot Venus surface with an average surface temperature of about 698 K.
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VenSpec-M will provide near-global compositional data on rock types, weathering, and crustal evolution by mapping the Venus surface in five atmospheric windows.
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