P065-0013
Nitrogen Fixation at Early Mars

Tuesday, 15 December 2020
Poster
Danica Adams1, Yangcheng Luo1, Michael L. Wong2, Patrick Dunn3, Chuanfei Dong4, Renyu Hu5 and Yuk L Yung5, (1)California Institute of Technology, Division of Geological and Planetary Sciences, Pasadena, CA, United States, (2)University of Washington Seattle Campus, Department of Astronomy & Astrobiology Program, Seattle, United States, (3)UC Berkeley, Space Science Laboratory, Berkeley, CA, United States, (4)Princeton University, Princeton, NJ, United States, (5)California Institute of Technology, Pasadena, CA, United States
Abstract:
The Mars Science Laboratory (MSL) recently discovered nitrates near Gale Crater (eg., Stern et al., 2015; Sutter et al., 2017). One possible mechanism for ancient nitrate deposition at Mars is through HNOx formation and rain-out in the atmosphere, for which lightning-induced NO is the fundamental source. This study investigates nitrogen fixation in early Mars’ atmosphere, with implications for early Mars’ habitability. We consider a 1-bar atmosphere of background composition CO2 with abundances of N2, H2, and CH4 varied from 1–10% 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 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 (SEP) 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 analyze and will discuss the photochemical network (shown in the figure) that produces and destroys these species. 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 oceanic concentrations (as in the figure) of ~0.1–3 µM cyanide and ~0.1–100 nM nitrate, and the latter demonstrates a significant response to the presence of reduced species (H2 and CH4). HCN is critical for protein synthesis at concentrations > 0.01 M (eg., Holm and Neubeck, 2009), and our results suggest that secondary local concentration mechanisms would be required to attain astrobiologically relevant concentrations. Nitrates may act as high potential electron acceptors for early metabolisms, and our work derives concentrations that will be useful for other future laboratory studies to investigate the habitability of early Mars.