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The chlorine isotopic composition of the Moon: Insights from melt inclusions

机译:月亮的氯同位素组成:熔体夹杂物的见解

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The Moon exhibits a heavier chlorine (Cl) isotopic composition compared to the Earth. Several hypotheses have been put forward to explain this difference, based mostly on analyses of apatite in lunar samples complemented by bulk-rock data. The earliest hypothesis argued for Cl isotope fractionation during the degassing of anhydrous basaltic magmas on the Moon. Subsequently, other hypotheses emerged linking Cl isotope fractionation on the Moon with the degassing during the crystallization of the Lunar Magma Ocean (LMO). Currently, a variant of the LMO degassing model involving mixing between two end member components, defined by early-formed cumulates, from which mare magmas were subsequently derived, and a KREEP component, which formed towards the end of the LMO crystallization, seems to reconcile some existing Cl isotope data on lunar samples. To further ascertain the history of Cl in the Moon and to investigate any evolution of Cl during magma crystallization and emplacement events, which could help resolve the chlorine isotopic variation between the Earth and the Moon, we analysed the Cl abundance and its isotopic composition in 36 olivine- and pyroxene-hosted melt inclusions (MI) in five Apollo basalts (10020, 12004, 12040, 14072 and 15016). Olivine-hosted MI have an average of 3.3 +/- 1.4 ppm Cl. Higher Cl abundances (11.9 ppm on average) are measured for pyroxene-hosted MI, consistent with their formation at later stages in the crystallization of their parental melt compared to olivines. Chlorine isotopic composition (delta Cl-37) of MI in the five Apollo basalts have weighted averages of +12.8 +/- 2.4 parts per thousand and +10.1 +/- 3.2 parts per thousand for olivine- and pyroxene-hosted MI, respectively, which are statistically indistinguishable. These isotopic compositions are also similar to those measured in apatite in these lunar basalts, with the exception of sample 14072, which is known to have a distinct petrogenetic history compared to other mare ba
机译:与地球相比,月亮表现出较重的氯(Cl)同位素组合物。已经提出了几个假设来解释这种差异,主要基于散装岩石数据的月球样本中磷灰石的分析。在月球上脱气的无水玄武岩岩浆中,最早的假设争论Cl同位素分馏。随后,在月球(LMO)的结晶期间,在月球上引起Cl同位素分馏的其他假设在月球(LMO)的结晶期间。目前,涉及涉及混合的LMO脱气模型的变型,这些模型由早期累积定义,随后衍生MARE岩浆,以及朝向LMO结晶结束的kreep组分似乎可以协调有些现有的CL同位素数据在月球样本上。为了进一步确定月球中CL的历史,并在岩浆结晶和施加事件期间调查CL的任何演变,这有助于解决地球和月球之间的氯同位素变异,我们分析了36中的CL丰度及其同位素组成五个Apollo BASALTS(10020,12004,12040,14072和15016)中的橄榄石和辉石托管宿主熔体夹杂物(MI)。 orivine托管的MI平均为3.3 +/- 1.4 ppm cl。测量辉芬托管的Mi的较高的Cl丰度(平均11.9ppm),与橄榄石相比,它们在其亲本熔体结晶中的后阶段的形成一致。五个Apollo沼气中MI的氯同位素组合物(Delta Cl-37)分别具有α112.8+ / -2.4份+12.8 + / -2.4份的加权平均值,分别为橄榄石和辉石托管的Mi +10.1 +/- 3.2份。在统计上无法区分。这些同位素组合物也与在这些月球基础上以磷灰石中测量的那些相似,除了样品14072,与其他母马BA相比,已知具有不同的细胞生成历史

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