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A simple evolutional model of Habitable Zone around host stars with various mass and low metallicity

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Abstract

Habitable Zone (HZ) is defined as a life existence area, where water at the surface of the terrestrial planet is in liquid phase. This is caused by the balance of flux from the host star and effective radiative cooling with greenhouse effect of the planet. However, the flux varies according to evolutional phase of the host star. So, a simple but newest HZ model considering stellar mass range from 0.08 to 4.00 M⊙ has been proposed. It studies both at zero-age main sequence (ZAMS) and terminal-age main sequence (TMS) phases to examine persistence of HZ. By the way, it discusses the case of the metallicity like the Sun. Actually, it is interesting to study a HZ model considering host stars with low metallicity. So, we examine the effect of metallicity, following the precedent simple model. In our analysis, metallicity affects little for HZ orbital range at ZAMS, while it affects clearly in case of TMS. Since the inner and outer HZ boundaries at TMS are shifted outward especially in the mass range from 1.5 to 2.0 M⊙, we find persistent HZ is allowed above about 1.8 M⊙. The age of the universe is 13.8 Gyr, which is comparable to main sequence life time of about 0.8 M⊙ for the low metallicity case. Then, the effect of metallicity to estimate HZ of low metallicity host stars is important for the mass range from 0.8 to 1.8 M⊙.

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Acknowledgements

The authors would like to thank the anonymous referee for useful and fruitful suggestions that helped us to improve the original manuscript very much.

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Authors and Affiliations

  1. Department of Earth and Ocean Sciences, School of Applied Sciences, National Defense Academy of Japan, Yokosuka, 239-8686, Japan

    Midori Oishi & Hideyuki Kamaya

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  1. Midori Oishi
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  2. Hideyuki Kamaya
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Correspondence to Midori Oishi.

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Oishi, M., Kamaya, H. A simple evolutional model of Habitable Zone around host stars with various mass and low metallicity. Astrophys Space Sci 361, 66 (2016). https://doi.org/10.1007/s10509-016-2659-6

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