The Diversity of Venus-like Atmospheres on Exoplanets

Geochemical models of atmospheric formation and evolution predict that Venus-like atmospheres, dominated by CO2 and thicker than a few bars pressure, are among the most common secondary volcanic atmospheres to be produced on rocky exoplanets. Meanwhile, astronomical detection biases toward short period planets ensure than rocky exoplanets are commonly found orbiting their host stars within the hypothetical 'Venus Zone' - a zone bounded by the cosmic shoreline at its inner edge and the CO2-condensation line at its outer edge. In this talk, I will present the chemical diversity of Venus-like atmospheres from both of these perspectives: the diversity of Venus-like atmospheres predicted via geochemistry, and the diversity of photochemical disequilibrium processes reshaping these atmospheres across the range of planet-hosting stars that we observe via astronomy.