The Inner Boundary of the Habitable Zone for Earth-like Planets

Details The Inner Boundary of the Habitable Zone for Earth-like Planets The Inner Boundary of the Habitable Zone for Earth-like Planets

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aspc..430..545s&link_type=abstract

Pathways Towards Habitable Planets, proceedings of a workshop held 14 to 18 September 2009 in Barcelona, Spain. Edited by Vincen

Astronomy and Astrophysics

Astronomy

Scientific paper

The orbital region around a star where liquid water could exist on the surface of a terrestrial planet is usually defined as the Habitable Zone (HZ). We investigate the inner boundary of the HZ for different planetary scenarios with a one-dimensional radiative-convective model of the atmosphere. Our modeling approach involves the step-by-step increase of the incoming stellar flux and the subsequent iterative calculation of resulting changes in the atmospheric water vapour content and the radiative properties. Modeling results are presented for the influence of various planetary and atmospheric conditions on the inner boundary (water loss limit) of the HZs around a Sun-type star.

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