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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 isvery close to the star itself. For planets close to their stars, tidal heatingplays an important role in thermal and orbital evolutions, especially when theplanet orbit has a relatively large eccentricity. Although tidal heatinginteracts with the thermal state and orbit of the planet, such coupledcalculations for extrasolar planets around M star have not been conducted. Weperform coupled calculations using simple structural and orbital models, andanalyze the thermal state and habitability of a terrestrial planet. Consideringthis planet to be Martian sized, the tide heats up and partially melts themantle, maintaining an equilibrium state if the mass of the star is less than0.2 times the mass of the Sun and the initial eccentricity of the orbit is morethan 0.2. The reduction of heat dissipation due to the melted mantle allows theplanet to stay in the habitable zone for more than 10 Gyr even though theorbital distance is small. The surface heat flux at the equilibrium state isbetween that of Mars and Io. The thermal state of the planet mainly depends onthe initial value of the eccentricity and the mass of the star.

Thermal-orbital coupled tidal heating and habitability of Martian-sized extrasolar planets around M stars