Habitable zones around M-dwarfs
The habitability of planets around M-dwarfs is heavily debated, with a common argument against being the volatility of M-dwarfs and their heightened stellar activity which could sterilise nearby planets.
However, research conducted by [ Jun Yang et al ] suggests that the inclusion of cloud simulation could greatly increase the expected widths of the habitable zones for tidally-locked planets in M-dwarf systems.
Incorporating cloud systems into 1D radiative-convective transfer models for determining the inner edge of the habitable zone could double the stellar flux at which a tidally locked planet can be considered habitable - effectively doubling the number of habitable planets around M dwarfs.
High stellar flux at the surface of a planet with plentiful water drives strong convection producing thick water clouds that increase planetary albedo. As cloud formation is also greater at areas with high insolation, this produces a stabilising feedback loop.
Research by J Yang et al. suggests that tidally locked planets have a higher albedo, lower greenhouse effect, and therefore temperatures low enough to be considered habitable. The temperature difference across the day and night sides of the planet is also mitigated by strong radiative cooling on the night side and atmospheric energy transport from the day side to the night side.