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The habitable zone (HZ) is the circumstellar region where a planet cansustain surface liquid water. Searching for terrestrial planets in the HZ ofnearby stars is the stated goal of ongoing and planned extrasolar planetsurveys. Previous estimates of the inner edge of the HZ were based onone-dimensional radiative-convective models. The most serious limitation ofthese models is the inability to predict cloud behavior. Here we use globalclimate models with sophisticated cloud schemes to show that due to astabilizing cloud feedback, tidally locked planets can be habitable at twicethe stellar flux found by previous studies. This dramatically expands the HZand roughly doubles the frequency of habitable planets orbiting red dwarfstars. At high stellar flux, strong convection produces thick water clouds nearthe substellar location that greatly increase the planetary albedo and reducesurface temperatures. Higher insolation produces stronger substellar convectionand therefore higher albedo, making this phenomenon a stabilizing climatefeedback. Substellar clouds also effectively block outgoing radiation from thesurface, reducing or even completely reversing the thermal emission contrastbetween dayside and nightside. The presence of substellar water clouds and theresulting clement surface conditions will therefore be detectable with theJames Webb Space Telescope.

Stabilizing Cloud Feedback Dramatically Expands the Habitable Zone of Tidally Locked Planets