Water is a fundamental molecule in the universe. On Earth, water exists in all three phases:
gas, liquid, and solid (ice). Liquid water facilitates many chemical reactions as a solvent …

This paper deals with the composition and chemical processes occurring in the neutral
atmosphere of Venus. Since the last synthesis, observers as well as modellers have …

A global-mean model of coupled neutral and ion chemistry on Titan has been developed.
Unlike the previous coupled models, the model involves ambipolar diffusion and escape of …

The NOMAD spectrometer suite on the ExoMars Trace Gas Orbiter will map the composition
and distribution of Mars׳ atmospheric trace species in unprecedented detail, fulfilling many …

Self‐consistent models for 11 neutral and 18 ion species from 80 to 300 km on Mars have
been developed by solving the continuity equations including ambipolar diffusion for ions …

Sea surface reservoir ages must be known to establish a common chronological framework
for marine, continental, and cryospheric paleoproxies, and are crucial for understanding …

Spectroscopy for the investigation of the characteristics of the atmosphere of Venus
(SPICAV) is a suite of three spectrometers in the UV and IR range with a total mass of 13.9 …

We present the first three‐dimensional model simulations of ozone on Mars. The model
couples a state‐of‐the‐art gas‐phase photochemical package to the general circulation …

The current Martian atmosphere is about five times more enriched in deuterium than Earth's,
providing direct testimony that Mars hosted vastly more water in its early youth than …

Venus has thick clouds of H2SO4 aerosol particles extending from altitudes of 40 to 60 km.
The 60–100 km region (the mesosphere) is a transition region between the 4 day retrograde …