Response comment: Carbon sequestration on Mars

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Martian atmospheric pressure has important implications for the past and present habitability of the planet, including the timing and causes of environmental change. The ancient Martian surface is strewn with evidence for early water bound in minerals (e.g., Ehlmann and Edwards, 2014) and recorded in surface features such as large catastrophically created outflow channels (e.g., Carr, 1979), valley networks (Hynek et al., 2010; Irwin et al., 2005), and crater lakes (e.g., Fassett and Head, 2008). Using orbital spectral data sets coupled with geologic maps and a set of numerical spectral analysis models, Edwards and Ehlmann (2015) constrained the amount of atmospheric sequestration in early Martian rocks and found that the majority of this sequestration occurred prior to the formation of the early Hesperian/late Noachian valley networks (Fassett and Head, 2011; Hynek et al., 2010), thus implying the atmosphere was already thin by the time these surface-water-related features were formed.

Publication type Article
Publication Subtype Journal Article
Title Response comment: Carbon sequestration on Mars
Series title Geology
DOI 10.1130/G37984Y.1
Volume 44
Issue 6
Year Published 2016
Language English
Publisher Geological Society of America
Publisher location Boulder, CO
Contributing office(s) Astrogeology Science Center
Description e389; 1 p.
Other Geospatial Mars
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