Nitrogen Fixation at Early Mars
Abstract
The Mars Science Laboratory (MSL) recently discovered nitrates in Gale Crater (e.g., Stern et al., 2015; Sutter et al., 2017). One possible mechanism for ancient nitrate deposition on Mars is through HNOx formation and rain out in the atmosphere, for which lightning-induced NO is likely the fundamental source. This study investigates nitrogen (N₂) fixation in early Mars' atmosphere, with implications for early Mars' habitability. We consider a 1 bar atmosphere of background CO₂, with abundance of N₂, hydrogen, and methane varied from 1% to 10% to explore a swath of potential early Mars climates. We derive lightning-induced thermochemical equilibrium fluxes of NO and HCN by coupling the lightning-rate parametrization from the study of Romps et al. (2014) with chemical equilibrium with applications, and we use a Geant4 simulation platform to estimate the effect of solar energetic particle events. These fluxes are used as input into KINETICS, the Caltech/JPL coupled photochemistry and transport code, which models the chemistry of 50 species linked by 495 reactions to derive rain-out fluxes of HNOx and HCN. We compute equilibrium concentrations of cyanide and nitrate in a putative northern ocean at early Mars, assuming hydrothermal vent circulation and photoreduction act as the dominant loss mechanisms. We find average oceanic concentrations of ∼0.1–2 nM nitrate and ∼0.01–2 mM cyanide. HCN is critical for protein synthesis at concentrations >0.01 M (e.g., Holm and Neubeck, 2009), and our result is astrobiologically significant if secondary local concentration mechanisms occurred. Nitrates may act as high-potential electron acceptors for early metabolisms, although the minimum concentration required is unknown. Our study derives concentrations that will be useful for future laboratory studies to investigate the habitability at early Mars. The aqueous nitrate concentrations correspond to surface nitrate precipitates of ∼1–8 × 10⁻⁴ wt % that may have formed after the evaporation of surface waters, and these values roughly agree with recent MSL measurements.
Additional Information
© 2021, Mary Ann Liebert, Inc., publishers. Submitted 7 April 2020; Accepted 26 April 2021. Online Ahead of Print: July 30, 2021. We thank Pin Chen, Armin Kleinboehl, Robin Wordsworth, David Romps, Stuart Bartlett, and Rob Lillis for useful discussions. D.A. was supported by NASA's FINESST program under Proposal Number 80NSSC19K1548. M.L.W. was supported by NASA's Virtual Planetary Laboratory under NASA Astrobiology Institute Cooperative Agreement Number NNA13AA93A and Grant Number 80NSSC18K0829. C.D. was supported by NASA's Habitable Worlds program under Proposal Number 80NSSC18K0288. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). This research was initiated under and partially supported by a NASA Habitable Worlds grant (#NNN130466T, later changed to #80NM0018F0612) to Pl R.H. and Co-I Y.L.Y. No competing financial interests exist.Attached Files
Published - ast.2020.2273_pub.pdf
Supplemental Material - Supp_AppS1.doc
Supplemental Material - Supp_AppS2.doc
Supplemental Material - Supp_AppS3.doc
Supplemental Material - Supp_AppS4.doc
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Additional details
- Eprint ID
- 110680
- DOI
- 10.1089/ast.2020.2273
- Resolver ID
- CaltechAUTHORS:20210831-224223138
- NASA Earth and Space Science and Technology Fellowship
- 80NSSC19K1548
- NASA
- NNA13AA93A
- NASA
- 80NSSC18K0829
- NASA
- 80NSSC18K0288
- NASA
- 80NM0018D0004
- NASA
- NNN130466T
- NASA
- 80NM0018F0612
- Created
-
2021-08-31Created from EPrint's datestamp field
- Updated
-
2021-08-31Created from EPrint's last_modified field
- Caltech groups
- Division of Geological and Planetary Sciences