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早期火星的氮固定。

Nitrogen Fixation at Early Mars.

机构信息

Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA.

Department of Astronomy and Astrobiology Program, University of Washington, Seattle, Washington, USA.

出版信息

Astrobiology. 2021 Aug;21(8):968-980. doi: 10.1089/ast.2020.2273. Epub 2021 Jul 30.

Abstract

The Mars Science Laboratory (MSL) recently discovered nitrates in Gale Crater (, Stern , 2015; Sutter , 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 (N) fixation in early Mars' atmosphere, with implications for early Mars' habitability. We consider a 1 bar atmosphere of background CO, with abundance of N, 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 (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 (, 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 wt % that may have formed after the evaporation of surface waters, and these values roughly agree with recent MSL measurements.

摘要

火星科学实验室(MSL)最近在盖尔陨石坑(Stern,2015 年;Sutter,2017 年)中发现了硝酸盐。火星古代硝酸盐沉积的一个可能机制是通过 HNOx 在大气中的形成和雨析,其中闪电诱导的 NO 可能是基本来源。本研究调查了早期火星大气中的氮(N)固定,这对早期火星的可居住性有影响。我们考虑了一个 1 巴的背景 CO 大气,其中 N、氢和甲烷的丰度从 1%变化到 10%,以探索一系列潜在的早期火星气候。我们通过将 Romps 研究中的闪电率参数化(2014 年)与化学平衡相结合,并使用 Geant4 模拟平台来估计太阳高能粒子事件的影响,来推导闪电诱导的 NO 和 HCN 热化学平衡通量。这些通量被用作 KINETICS 的输入,这是一个由加州理工学院/喷气推进实验室联合开发的光化学和运输代码,它模拟了 50 种物质的化学,这些物质通过 495 个反应连接起来,以推导 HNOx 和 HCN 的雨析通量。我们假设热液喷口循环和光还原作用是主要的损耗机制,在早期火星的一个假设的北部海洋中计算了氰化物和硝酸盐的平衡浓度。我们发现,海洋的平均浓度约为 0.1-2 nM 硝酸盐和约 0.01-2 mM 氰化物。HCN 在浓度 >0.01 M 时对蛋白质合成至关重要(Holm 和 Neubeck,2009),如果发生了二级局部浓缩机制,我们的结果在天体生物学上是有意义的。硝酸盐可能作为早期新陈代谢的高潜力电子受体,尽管所需的最低浓度尚不清楚。我们的研究得出的浓度将有助于未来的实验室研究,以调查早期火星的可居住性。水合硝酸盐浓度对应于表面硝酸盐沉淀物的约 1-8 × 10wt%,这些沉淀物可能是在表面水蒸发后形成的,这些值与最近的 MSL 测量值大致相符。

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