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The potential habitability of a terrestrial planet is usually defined by thepossible existence of liquid water on its surface. The potential presence ofliquid water depends on many factors such as, most importantly, surfacetemperatures. The properties of the planetary atmosphere and its interactionwith the radiative energy provided by the planet's host star are thereby ofdecisive importance. In this study we investigate the influence of differentmain-sequence stars upon the climate of Earth-like extrasolar planets and theirpotential habitability by applying a 3D Earth climate model accounting forlocal and dynamical processes. The calculations have been performed for planetswith Earth-like atmospheres at orbital distances where the total amount ofenergy received from the various host stars equals the solar constant. Incontrast to previous 3D modeling studies, we include the effect of ozoneradiative heating upon the vertical temperature structure of the atmospheres.The global orbital mean results obtained have been compared to those of a 1Dradiative convective climate model. The different stellar spectral energydistributions lead to different surface temperatures and due to ozone heatingto very different vertical temperature structures. As previous 1D studies wefind higher surface temperatures for the Earth-like planet around the K-typestar, and lower temperatures for the planet around the F-type star compared toan Earth-like planet around the Sun. However, this effect is more pronounced inthe 3D model results than in the 1D model because the 3D model accounts forfeedback processes such as the ice-albedo and the water vapor feedback. Whetherthe 1D model may approximate the global mean of the 3D model results stronglydepends on the choice of the relative humidity profile in the 1D model, whichis used to determine the water vapor profile.

3D climate modeling of Earth-like extrasolar planets orbiting different types of host stars