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首页> 美国卫生研究院文献>International Journal of Molecular Sciences >Academic Aspects of Lunar Water Resources and Their Relevance to Lunar Protolife
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Academic Aspects of Lunar Water Resources and Their Relevance to Lunar Protolife

机译：月球水资源的学术方面及其与月球原生生物的关系

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Water ice has been discovered on the moon by radar backscatter at the North Pole and by spectrometry at the South Pole in the Cabeus crater with an extrapolated volume for both poles of conservatively 109 metric tons. Various exogenic and endogenic sources of this water have been proposed. This paper focuses on endogenic water sources by fumaroles and hot springs in shadowed polar craters. A survey of theoretical and morphological details supports a volcanic model. Release of water and other constituents by defluidization over geological time was intensified in the Hadean Eon (c.a. 4600 to 4000 My). Intensification factors include higher heat flow by now-extinct radionuclides, tidal flexing and higher core temperatures. Lesser gravity would promote deeper bubble nucleation in lunar magmas, slower rise rates of gases and enhanced subsidence of lunar caldera floors. Hadean volcanism would likely have been more intense and regional in nature as opposed to suture-controlled location of calderas in Phanerozoic Benioff-style subduction environments. Seventy-seven morphological, remote sensing and return sample features were categorized into five categories ranging from a volcano-tectonic origin only to impact origin only. Scores for the most logical scenario were 69 to eight in favor of lunar volcanism. Ingredients in the Cabeus plume analysis showed many volcanic fluids and their derivatives plus a large amount of mercury. Mercury-rich fumaroles are well documented on Earth and are virtually absent in cometary gases and solids. There are no mercury anomalies in terrestrial impact craters. Volcanic fluids and their derivatives in lunar shadow can theoretically evolve into protolife. Energy for this evolution can be provided by vent flow charging intensified in the lunar Hadean and by charge separation on freezing fumarolic fluids in shadow. Fischer-Tropsch reactions on hydrothermal clays can yield lipids, polycyclic aromatic hydrocarbons and amino acids. Soluble polyphosphates are available in volcanic fluids as well as vital catalysts such as tungsten. We conclude that the high volume of polar water resources supports the likelihood of lunar volcanism and that lunar volcanism supports the likelihood of protolife.
机译：在月球上，北极的雷达后向散射和卡贝斯火山口的南极的光谱法发现了水冰，两个极的推算体积保守地为10 9 公吨。已经提出了这种水的各种外源和内源来源。本文重点研究了阴影极地火山口中的喷气孔和温泉产生的内生水源。对理论和形态学细节的调查支持了火山模型。在Hadean Eon（约4600到4000 My）中，随着地质时间的流逝，水和其他成分的释放得到加强。增强因素包括现在已灭绝的放射性核素带来的更高的热流，潮汐弯曲和更高的岩心温度。较小的重力将促进月球岩浆中更深的气泡成核，降低气体的上升速度并增强月球破火山口地板的沉降。与Phanerozoic Benioff式俯冲环境中火山口的缝合控制位置不同，Hadean火山活动本来可能会更加激烈和区域化。 77个形态，遥感和返回样本特征被分为五类，从仅火山构造起源到仅撞击起源。在最合乎逻辑的情况下，赞成月球火山活动的得分为69至8。 Cabeus羽流分析中的成分显示出许多火山岩液及其衍生物以及大量的汞。富含汞的喷气孔在地球上有据可查，并且在彗星气体和固体中几乎不存在。地面撞击坑内没有汞异常。理论上，月球阴影中的火山流体及其衍生物可以进化为原生生物。这种演化的能量可以通过在哈德族月球上增强的排气流量以及阴影中冷冻的富马酸流体的电荷分离来提供。在热液粘土上的费-托反应可产生脂质，多环芳烃和氨基酸。火山岩液以及重要的催化剂（例如钨）中都有可溶性多磷酸盐。我们得出的结论是，大量的极地水资源支持月球火山活动的可能性，而月球火山活动则支持原生物的可能性。

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