![Vertical velocity and condensate cross-sections in (x,z) taken in the middle of the y-domain for the adiabatic simulation initialized on the moist adiabat. The top row shows the vertical velocity in [m/s] at different times throughout the CM1 simulation. The bottom row shows the condensate mixing ratio in [g/kg] at different times throughout the CM1 simulation. The vertical velocity cross-sections show clear convective inhibition in the lower atmosphere in all time steps. The corresponding condensate mixing ratio show a condensate formation nearly in the whole domain, but re-evaporation occurs at the boundary between the stable and convection regions. -- astro-ph.EP](https://i0.wp.com/astrobiology.com/wp-content/uploads/2024/10/3D-Modeling-of-Moist-Convective-Inhibition.png?resize=1200%2C718&ssl=1)
Many planets have hydrogen-dominated atmospheres, including sub-Neptune exoplanets, recently formed planets with primordial atmospheres, and the Solar System’s giant planets. Atmospheric convection behaves differently in hydrogen-rich atmospheres compared to higher […]
hydrogen-dominated atmosphere
Posted inAtmospheres, Climate, Weather, Biogeochemical Cycles & Geobiology, Biosignatures & Paleobiology, Exoplanets, -moons, -comets, Habitable Zones, Imaging & Spectroscopy, Status Report, Water/Hycean Worlds & Oceanography
Biogenic Sulfur Gases As Biosignatures On Temperate Sub-Neptune Waterworlds
Theoretical predictions and observational data indicate a class of sub-Neptune exoplanets may have water-rich interiors covered by hydrogen-dominated atmospheres. Provided suitable climate conditions, such planets could host surface liquid oceans.