More than three decades have passed since the publication of the last review of the Venus
clouds and hazes. The paper published in 1983 in the Venus book summarized the …

Surface mineralogy records the primary composition, climate history and the geochemical
cycling between the surface and atmosphere. We have not yet directly measured mineralogy …

The recent candidate detection of∼ 1 ppb of phosphine in the middle atmosphere of Venus
is so unexpected that it requires an exhaustive search for explanations of its origin …

The depletion of SO 2 and H 2 O in and above the clouds of Venus (45–65 km) cannot be
explained by known gas-phase chemistry and the observed composition of the atmosphere …

We model the formation of silicate atmospheres on hot volatile-free super-Earths. Our
calculations assume that all volatile elements such as H, C, N, S, and Cl have been lost from …

We show that solar irradiances calculated across Venus' clouds support the potential for
Earth-like phototrophy and that treatment of Venus' aerosols containing neutralized sulfuric …

The upcoming launch of the James Webb Space Telescope means that we will soon have
the capability to characterize the atmospheres of rocky exoplanets. However, it is still …

Despite its importance in geological sciences, our understanding of interactions between
gas and condensed phases (comprising solids and liquids) remains clouded by the fact that …

Abstract Gold-(silver)-telluride (selenide) ores occur as epithermal orogenic and intrusion
related deposits. Although Te and Se are chalcophile elements and share geochemical …

Gas–solid reactions on solar system bodies occur in the vicinity of their surfaces and in their
interiors where gases are liberated through magma degassing or thermal devolatilization …