Is there a habitable zone around M and late K-type stars?

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The habitable zone (HZ) is the circumstellar region where the greenhouse effect of a planetary atmosphere can provide surface temperatures above the freezing point of water. The inner and outer limits of the HZ depend on the total stellar luminosity (Lbol) and the planet's orbital distance. In the case of M and late K-type stars, the HZ is much closer to the host star than in the case of solar-type G stars because the total stellar luminosity is significantly lower (<10%). Observations show that late K and M-type stars are very active in the EUV-X region and have a ratio LX/Lbol of nearly 10-3 during the first few Gyr of their lifes. LX/Lbol for solar type stars can also be as high for ages below 100~Myr but it decreases rapidly to a value of about 10-5 in less than 1 Gyr. The high X-EUV irradiation heats dramatically the upper layer (exosphere) of the planetary atmospheres, inducing a strong thermal escape that could affect not only H and He, but also the main constituents of the atmosphere (N, C, O). We investigate thermal escape on terrestrial planets around M and late K-type stars in order to estimate the loss rate of gases for various atmospheric compositions and to put constraints on habitability.

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