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Terrestrial-type exoplanets orbiting nearby red dwarf stars (M-dwarfs) areamong the best targets for atmospheric characterization and biosignaturesearches in the near future. Recent evolutionary studies have suggested thatterrestrial planets in the habitable zone of M-dwarfs are probably tidallylocked and have limited surface water inventories as a result of their hoststars' high early luminosities. Several previous climate simulations of suchplanets have indicated that their remaining water would be transported to theplanet's permanent nightside and become trapped as surface ice, leaving thedayside devoid of water. Here we use a three-dimensional general circulationmodel with a water cycle and accurate radiative transfer scheme to investigatethe surface water evolution on slowly rotating tidally locked terrestrialplanets with limited surface water inventories. We show that there is acompetition for water trapping between the nightside surface and the substellartropopause in this type of climate system. Although under some conditions thesurface water remains trapped on the nightside as an ice sheet, in other casesliquid water stabilizes in a circular area in the substellar region as awetland. Planets with 1 bar N$_2$ and atmospheric CO$_2$ levels greater than0.1 bar retain stable dayside liquid water, even with very small surface waterinventories. Our results reveal the diversity of possible climate states onterrestrial-type exoplanets and highlight the importance of surface liquidwater detection techniques for future characterization efforts.

Stabilization of dayside surface liquid water via tropopause cold trapping on arid slowly rotating tidally locked planets