M type stars are good targets in the search for habitable extrasolar planets. Because of their low effective temperatures, the habitable zone of M stars is very close to the star itself.
For planets close to their stars, tidal heating plays an important role in thermal and orbital evolutions, especially when the planet orbit has a relatively large eccentricity. Although tidal heating interacts with the thermal state and orbit of the planet, such coupled calculations for extrasolar planets around M star have not been conducted.
We perform coupled calculations using simple structural and orbital models, and analyze the thermal state and habitability of a terrestrial planet. Considering this planet to be Martian sized, the tide heats up and partially melts the mantle, maintaining an equilibrium state if the mass of the star is less than 0.2 times the mass of the Sun and the initial eccentricity of the orbit is more than 0.2. The reduction of heat dissipation due to the melted mantle allows the planet to stay in the habitable zone for more than 10 Gyr even though the orbital distance is small.
The surface heat flux at the equilibrium state is around 0.2 W m2 , which is between that of Mars and Io. The thermal state of the planet mainly depends on the initial value of the eccentricity and the mass of the star, which can be estimated from the observation.
Daigo Shoji, Kei Kurita (Submitted on 11 Feb 2014)
Comments: 24 pages, 5 figures, 1 table, submitted to ApJ
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:1402.2378 [astro-ph.EP] (or arXiv:1402.2378v1 [astro-ph.EP] for this version)
Submission history From: Daigo Shoji [v1] Tue, 11 Feb 2014 05:43:35 GMT (262kb)
Please follow Astrobiology on Twitter.