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Re-Evaluation of the Inner Edge of Habitable Zone

Published online by Cambridge University Press:  29 April 2014

Takanori Kodama ,
Hidenori Genda ,
Yutaka Abe  and
Kevin Zahnle
Takanori Kodama
Affiliation:
Department of Earth and Planetary Science, The University of Tokyo, 7-3-1, Hongo, Bunkyo-ku, Tokyo, Japan email: koda@eps.s.u-tokyo.ac.jp
Hidenori Genda
Affiliation:
Earth-Life Science Institute, Tokyo institute of Technology, 2-12-lE-1, Ookayama, Meguro-ku, Tokyo, Japan
Yutaka Abe
Affiliation:
Department of Earth and Planetary Science, The University of Tokyo, 7-3-1, Hongo, Bunkyo-ku, Tokyo, Japan email: koda@eps.s.u-tokyo.ac.jp
Kevin Zahnle
Affiliation:
NASA Ames Research Center, Moffett Field, California, USA
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Abstract

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Existence of liquid water on the planetary surface is thought to be an important condition for the origin and evolution of life. Planets with oceans (or lakes) are classified in two types: Earth-like ‘aqua planets’ and less water ‘land planets’. The latter shows stronger resistance than the former to the runaway greenhouse caused by the increase of stellar luminosity. We examined the possibility of evolution from an aqua planet to a land planet by water loss. We showed that an aqua planet with less than about 0.1 present Earth's ocean mass can evolve to a land planet without having experience of the runaway greenhouse, and maintains liquid water on its surface for about 2Gyrs longer than planets with larger amount of water. Our results mean that the initial amount of water is important for their evolution paths and habitability.

Keywords

HabitabilityHabitable Zonestellar insolation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S293: Formation, Detection, and Characterization of Extrasolar Habitable Planets , August 2012 , pp. 323 - 325
Copyright
Copyright © International Astronomical Union 2014 

References

Abe, Y. & Matsui, T. 1988, J Atmos Sci 45 3801–3101Google Scholar
Abe, Y., Abe-Ouchi, A., Sleep, N. H., & Zahnle, K. 2011, Astrobiology 11 443–460Google Scholar
Gough, D. O. 1981, Solar Physics 74 21–34Google Scholar
Kasting, J. F., Whitmire, D. P., & Reynolds, R. T. 1993, Icarus 101 108–128CrossRefGoogle Scholar
Kopparapu, , et al. 2013, ApJ, 765, 131Google Scholar
Lammer, , et al. 2009, A&A 506 399–410Google Scholar
Walker, J. C. G. 1977, Evolution of the Atmosphere. MacMillan, New York, p.164Google Scholar
Watson, A. J., Donahue, T. M., & Walker, J. C. G. 1981, Icarus 48 150–166Google Scholar