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首页> 外文期刊>Earth and Planetary Science Letters: A Letter Journal Devoted to the Development in Time of the Earth and Planetary System >Preservation of primordial signatures of water in highly-shocked ancient lunar rocks
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Preservation of primordial signatures of water in highly-shocked ancient lunar rocks

机译：在高度震惊的古老月球岩中保存水的原始签名

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Spurred by the discovery of water in lunar volcanic glasses about a decade ago, the accessory mineral apatite became the primary target to investigate the abundance and source of lunar water. This is due to its ability to contain significant amounts of OH in its structure, along with the widespread presence of apatite in lunar rocks. There is a general understanding that crustal cumulate rocks of the lunar magnesian (Mg) suite are better candidates for recording the original isotopic compositions of volatile elements in their parental melts compared to eruptive rocks, such as mare basalts. Consequently, water-bearing minerals in Mg-suite rocks are thought to be ideal candidates for discerning the primary hydrogen isotopic composition of water in the lunar interior. Mg-suite rocks and most other Apollo samples that were collected at the lunar surface display variable degrees of shock-deformation. In this study, we have investigated seven Apollo 17 Mg-suite samples that include troctolite, gabbro and norite lithologies, in order to understand if shock processes affected the water abundances and/or H isotopic composition of apatite. The measured water contents in apatite grains range from 31 to 964 ppm, with associated SD values varying between -535 +/- 134 parts per thousand and +147 +/- 194 parts per thousand (2 sigma). Considering the full dataset, there appears to be no correlation between H2O and delta D of apatite and the level of shock each apatite grain has experienced. However, the lowest delta D was recorded by individual, water-poor (similar to 100 ppm H2O), regardless of the complexity of the shock-induced nanostructures, there appears to be no evidence of water-loss or alteration in their delta D. The weighted average delta D value of 24 such water-rich apatites is -192 +/- 71 parts per thousand, and, of all 36 analyzed spots is -209 +/- 47 parts per thousand, indistinguishable from that of other KREEPy lunar lithologies or the Earth's deep mantle. Despite experiencing variable degrees of shock-deformation at a later stage in lunar history, water-rich apatite in some of the earliest-formed lunar crustal material appears to retain the original isotopic signature of H in the Moon. (C) 2020 The Author(s). Published by Elsevier B.V.
机译：通过水在大约十年前的月球火山玻璃的发现刺激下，该副矿物磷灰石成为首要目标，调查的月球水的数量和来源。这是因为它含有大量显著OH在其结构，磷灰石的月球岩石中广泛存在一起的能力。有一个一般的理解是，月球镁（Mg）的套件的地壳岩石累积是相比喷发岩，如海玄武岩记录挥发性元素的原始同位素组成在它们的亲本熔体更好的候选者。因此，在Mg的套房岩含水矿物被认为是用于辨别的水的主要的氢同位素组成在月球内部的理想候选物。 Mg的套件岩石和其他大多数阿波罗样品收集在月球表面显示不同程度的冲击变形的那个。在这项研究中，我们已经调查7阿波罗17的Mg-套件样品包括橄长岩，辉长岩和苏长岩岩性，以了解是否休克过程影响了水的丰度和/或磷灰石的氢同位素组成。在磷灰石粒所测得的水含量范围为31至964 ppm的，具有相关联的值SD +/- -535 134份‰，每千（2西格马）147 +/- 194份之间变化。考虑完整数据集，似乎存在H 2 O和磷灰石的增量d和各晶粒磷灰石经历了震动的水平之间没有相关性。但是，最低的增量d是由个人，贫水（<类似于100ppm的H 2 O）磷灰石颗粒是直接与冲击接触熔化或在其附近记录。因此，磷灰石的低-Δd的签名可以是具有d-差风化层（太阳风衍生1H），由可能对挥发物的迁移提供传导途径休克诱导的纳米结构促进相互作用的结果。相反，在相对富含水的磷灰石（>类似于100ppm的H 2 O），而不管该冲击引起的纳米结构的复杂性，存在似乎没有水损失或改变的证据在其增量D.加权平均增量的24个这样的富含水的磷灰石d值是每千-192 +/- 71份，和，所有36个分析点的是每千-209 +/- 47份，将其与其它KREEPy月球岩性或地球深区分地幔。尽管在月球历史的稍后阶段经历了不同程度的冲击，变形的，在一些最早形成的月球地壳物质的富水磷灰石似乎保留H的原同位素特征在月亮。 （c）2020提交人。由elsevier b.v出版。

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