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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 >Origin of hydrogen isotopic variations in chondritic water and organics
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Origin of hydrogen isotopic variations in chondritic water and organics

机译：软体病水和有机物中的氢同位素变异的起源

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摘要

Chondrites are rocky fragments of asteroids that formed at different times and heliocentric distances in the early solar system. Most chondrite groups contain water-bearing minerals, attesting that both water-ice and dust were accreted on their parent asteroids. Nonetheless, the hydrogen isotopic composition (D/H) of water in the different chondrite groups remains poorly constrained, due to the intimate mixture of hydrated minerals and organic compounds, the other main H-bearing phase in chondrites. Building on our recent works using in situ secondary ion mass spectrometry analyses, we determined the H isotopic composition of water in a large set of chondritic samples (CI, CM, CO, CR, and C-ungrouped carbonaceous chondrites) and report that water in each group shows a distinct and unique D/H signature. Based on a comparison with literature data on bulk chondrites and their water and organics, our data do not support a preponderant role of parent-body processes in controlling the D/H variations among chondrites. Instead, we propose that the water and organic D/H signatures were mostly shaped by interactions between the protoplanetary disk and the molecular cloud that episodically fed the disk over several million years. Because the preservation of D-rich interstellar water and/or organics in chondritic materials is only possible below their respective sublimation temperatures (160 and 350-450 K), the H isotopic signatures of chondritic materials depend on both the timing and location at which their parent body formed. (C) 2021 Elsevier B.V. All rights reserved.
机译：球粒陨石是早期太阳系中不同时间和日心距离形成的小行星的岩石碎片。大多数球粒陨石群都含有含水矿物，证明水冰和尘埃都是在它们的母小行星上堆积的。尽管如此，由于水合矿物和有机化合物（球粒陨石中的另一个主要含氢相）的紧密混合物，不同球粒陨石群中水的氢同位素组成（D/H）仍然受到很好的限制。在我们最近的一系列碳同位素分析中，我们在水和碳同位素分析中确定了每个碳粒陨石的独特组分。基于与有关大块球粒陨石及其水和有机物的文献数据的比较，我们的数据不支持母体过程在控制球粒陨石中D/H变化方面的主导作用。相反，我们提出，水和有机D/H特征主要是由原行星盘和分子云之间的相互作用形成的，这些分子云在数百万年的时间里间歇性地向该盘提供能量。由于球粒陨石中富含D的星际水和/或有机物只能在各自的升华温度（160和350-450 K）以下保存，因此球粒陨石的H同位素特征取决于其母体形成的时间和位置。（c）2021爱思唯尔B.V.保留所有权利。

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