Planetary Atmosphere Stability in the Habitable Zones of M-stars

Details Planetary Atmosphere Stability in the Habitable Zones of M-stars Planetary Atmosphere Stability in the Habitable Zones of M-stars

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p11a1336t&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #P11A-1336

Biology

[5210] Planetary Sciences: Astrobiology / Planetary Atmospheres, Clouds, And Hazes

Scientific paper

The traditional habitable zone depends on conditions suitable for long term stability of liquid water on the surface of planets. It is suggested that the frequent intense stellar CME events could have led to so rapid erosion of planetary atmospheres that generally speaking there is essentially no habitable zones for Earth-mass planets around M-stars. However, fast atmospheric escape could be a self-limiting process from an energy conservation point of view. It is already shown that CO2-dominant planetary atmospheres are stable in the habitable zones of M-stars. What about atmospheres with other compositions? In this work we will explore the atmosphere stability of planets with different mass and atmospheric composition in the habitable zones of M-stars.

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