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H$_2$O is a key molecule in characterizing atmospheres of temperateterrestrial planets, and observations of transmission spectra are expected toplay a primary role in detecting its signatures in the near future. Thedetectability of H$_2$O absorption features in transmission spectra depends onthe abundance of water vapor in the upper part of the atmosphere. We study thethree-dimensional distribution of atmospheric H$_2$O for synchronously rotatingEarth-sized aquaplanets using the general circulation model (GCM) ROCKE-3D, andexamine the effects of total incident flux and stellar spectral type. Weobserve a more gentle increase of the water vapor mixing ratio in response toincreased incident flux than one-dimensional models suggest, in qualitativeagreement with the climate-stabilizing effect of clouds around the substellarpoint previously observed in GCMs applied to synchronously rotating planets.However, the water vapor mixing ratio in the upper atmosphere starts toincrease while the surface temperature is still moderate. This is explained bythe circulation in the upper atmosphere being driven by the radiative heatingdue to absorption by water vapor and cloud particles, causing efficientvertical transport of water vapor. Consistently, the water vapor mixing ratiois found to be well-correlated with the near-infrared portion of the incidentflux. We also simulate transmission spectra based on the GCM outputs, and showthat for the more highly irradiated planets, the H$_2$O signatures may bestrengthened by a factor of a few, loosening the observational demands for aH$_2$O detection.

NIR-Driven Moist Upper Atmospheres of Synchronously Rotating Temperate Terrestrial Exoplanets