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As a contribution to the study of the habitability of extrasolar planets, weimplemented a 1-D Energy Balance Model (EBM), the simplest seasonal model ofplanetary climate, with new prescriptions for most physical quantities. Here weapply our EBM to investigate the surface habitability of planets with anEarth-like atmospheric composition but different levels of surface pressure.The habitability, defined as the mean fraction of the planet's surface on whichliquid water could exist, is estimated from the pressure-dependent liquid watertemperature range, taking into account seasonal and latitudinal variations ofsurface temperature. By running several thousands of EBM simulations wegenerated a map of the habitable zone (HZ) in the plane of the orbitalsemi-major axis, a, and surface pressure, p, for planets in circular orbitsaround a Sun-like star. As pressure increases, the HZ becomes broader, with anincrease of 0.25 AU in its radial extent from p=1/3 bar to p=3 bar. At lowpressure, the habitability is low and varies with a; at high pressure, thehabitability is high and relatively constant inside the HZ. We interpret theseresults in terms of the pressure dependence of the greenhouse effect, theeffciency of horizontal heat transport, and the extent of the liquid watertemperature range. Within the limits discussed in the paper, the results can beextended to planets in eccentric orbits around non-solar type stars. The maincharacteristics of the pressure-dependent HZ are modestly affected byvariations of planetary properties, particularly at high pressure.

The habitable zone of Earth-like planets with different levels of atmospheric pressure