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The habitable zone (HZ) describes the range of orbital distances around astar where the existence of liquid water on the surface of an Earth-like planetis in principle possible. While 3D climate studies can calculate the watervapor, ice albedo, and cloud feedback self-consistently and therefore allow fora deeper understanding and the identification of relevant climate processes, 1Dmodel studies rely on fewer model assumptions and can be more easily applied tothe large parameter space possible for exoplanets. We evaluate theapplicability of 1D climate models to estimate the potential habitability ofEarth-like exoplanets by comparing our 1D model results to those of 3D climatestudies in the literature. We applied a cloud-free 1D radiative-convectiveclimate model to calculate the climate of Earth-like planets around differenttypes of main-sequence stars with varying surface albedo and relative humidityprofile. These parameters depend on climate feedbacks that are not treatedself-consistently in most 1D models. We compared the results to those of 3Dmodel calculations in the literature and investigated to what extent the 1Dmodel can approximate the surface temperatures calculated by the 3D models. The1D parameter study results in a large range of climates possible for anEarth-sized planet with an Earth-like atmosphere and water reservoir at acertain stellar insolation. At some stellar insolations the full spectrum ofclimate states could be realized, i.e., uninhabitable conditions as well ashabitable surface conditions, depending only on the relative humidity andsurface albedo assumed. When treating the surface albedo and the relativehumidity profile as parameters in 1D model studies and using the habitabilityconstraints found by recent 3D modeling studies, the same conclusions about thepotential habitability of a planet can be drawn as from 3D model calculations.

Assessing the habitability of planets with Earth-like atmospheres with 1D and 3D climate modeling