Biosignature Gases in H2-Dominated Atmospheres on Rocky Exoplanets S
The Astrophysical Journal, 777:95 (19pp), 2013 November 10 doi:10.1088/0004-637X/777/2/95 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. BIOSIGNATURE GASES IN H2-DOMINATED ATMOSPHERES ON ROCKY EXOPLANETS S. Seager1,2,W.Bains1,3, and R. Hu1 1 Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA 2 Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA 3 Rufus Scientific Ltd., 37 The Moor, Melbourn, Herts SG8 6ED, UK Received 2013 April 2; accepted 2013 August 13; published 2013 October 18 ABSTRACT Super-Earth exoplanets are being discovered with increasing frequency and some will be able to retain stable H2- dominated atmospheres. We study biosignature gases on exoplanets with thin H2 atmospheres and habitable surface temperatures, using a model atmosphere with photochemistry and a biomass estimate framework for evaluating the plausibility of a range of biosignature gas candidates. We find that photochemically produced H atoms are the most abundant reactive species in H2 atmospheres. In atmospheres with high CO2 levels, atomic O is the major destructive species for some molecules. In Sun-Earth-like UV radiation environments, H (and in some cases O) will rapidly destroy nearly all biosignature gases of interest. The lower UV fluxes from UV-quiet M stars would produce a lower concentration of H (or O) for the same scenario, enabling some biosignature gases to accumulate. The favorability of low-UV radiation environments to accumulate detectable biosignature gases in an H2 atmosphere is closely analogous to the case of oxidized atmospheres, where photochemically produced OH is the major destructive species.
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