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 …

Oxygenic photosynthesis is Earth's dominant metabolism, having evolved to harvest the
largest expected energy source at the surface of most terrestrial habitable zone planets …

Photochemistry is a fundamental process of planetary atmospheres that regulates the
atmospheric composition and stability. However, no unambiguous photochemical products …

Mass-independent fractionation (MIF) of sulfur isotopes has been reported in sediments of
Archean and Early Proterozoic Age (> 2.3 Ga) but not in younger rocks. The only …

Updated chemical schemes and estimates of key rate coefficients are used in the present
investigation of the photochemistry of Titan atmosphere CH-and O-atom containing simple …

In the search for life on Earth-like planets around other stars, the first (and likely only)
information will come from the spectroscopic characterization of the planet's atmosphere. Of …

The habitability of the surface of any planet is determined by a complex evolution of its
interior, surface, and atmosphere. The electromagnetic and particle radiation of stars drive …

Proxima Centauri b provides an unprecedented opportunity to understand the evolution and
nature of terrestrial planets orbiting M dwarfs. Although Proxima Cen b orbits within its star's …

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 …

A one-dimensional photochemical-dynamic model is used to study hydrodynamic loss of
hydrogen from a primitive, water-rich atmosphere on Venus. The escape flux is calculated as …