Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.4202k&link_type=abstract
American Astronomical Society, ESS meeting #2, #42.02
Astronomy and Astrophysics
Astronomy
Scientific paper
Habitable zone (HZ) has been defined as the region from the central star where liquid water is stable in the planetary surface. Kasting et al. (1993) has estimated the width of HZ around various types of the main sequence stars for the Earth-like planets (called ‘aqua planet’). In the results, they estimated HZ; 90% - 110% of the present solar radiation at 1 AU.
Abe et al. (2011) has considered a hypothetical planet with very small amount of water (called ‘land planet’). Using the GCM (General Circulation Model), they found that HZ for a land planet is located between 77% and 170% of the present solar radiation at 1AU, which means that HZ for a land planet is about three times wider than that for an aqua planet.
Therefore, the amount of water on the planetary surface is important for the width of HZ. We focus on long term processes of water escape. If the water is efficiently lost during stellar age, there is a possibility that an aqua planet changes to a land planet which means that the HZ becomes wider. In this case, the aqua planet inside or outside of HZ would become habitable planets as a land planet.
On a hypothetical planet with various initial water contents and distances from central star, we calculate the evolution of water content on the planet and discuss planetary states by considering the hydrodynamic escape of water and star evolutions. In our results, in case of solar type stellar and a planet that initially possesses about 0.1ocean masses, planets change from the mode of aqua planet to the mode of land planet at about 0.7 AU. Our study demonstrates the possibility of the various types of habitable planets, which will be observed in the future.
Abe Yasuhiro
Genda Hidenori
Kodama Takanori
Zahnle Kevin J.
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