Understanding the formation of our planetary system requires identification of the materials from which it originated and the accretion processes that produced the planets. The compositional evolution of the solar system can be constrained by synthesizing astronomical datasets and numerical models with elemental and isotopic compositions from objects that directly sampled the disk: meteorites and their constituents (chondrules, refractory inclusions, and matrix). This contribution reviews constraints on early solar system evolution provided by the so-called non-carbonaceous (NC) and carbonaceous chondrite (CC) groups and their relationship to the volatile element characteristics of chondritic meteorites. In previous work, the NC or CC character of a parent body was used to infer its accretion location in the protoplanetary disk. The NC groups purportedly originated in the inner disk, and the CC groups were derived from the outer disk, where the NC and CC regions of the disk may have been separated early on by proto-Jupiter, a pressure maximum, or a dust trap in the disk. The tenet that all CC parent bodies accreted in the outer disk is, in part, based on evidence that a handful of CC meteorites are enriched in volatile species compared to NC meteorites. Here, it is reviewed if and how the volatile element and nucleosynthetic isotope compositions of meteorites can be linked to accretion locations within the disk. The nucleosynthetic isotope compositions of whole rock meteorite samples contrast the trends found for their major volatile element compositions (i.e., C, N, and O). Although there may be an increase in volatile abundances when comparing some stony NC and CC meteorites and their inferred accretion locations within the disk, this is not necessarily a general rule. The difficulties with inferring parent body accretion locations are discussed. It is found that it cannot always be assumed that parent bodies which formed in the CC reservoir are “volatile-rich” relative to those that formed in the NC reservoir which are “volatile-poor”. Consequently, tracing the origin of terrestrial volatiles using the NC-CC isotope dichotomy remains challenging.

中文翻译：

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NC-CC 同位素二分法：对早期太阳系化学和同位素演化的影响

了解我们行星系统的形成需要确定它起源的材料以及产生行星的吸积过程。太阳系的成分演化可以通过合成天文数据集和数值模型来限制，这些模型具有来自直接对圆盘采样的物体的元素和同位素成分：陨石及其成分（球粒、耐火包裹体和基质）。这篇文章回顾了所谓的非碳质 (NC) 和碳质球粒陨石 (CC) 群对早期太阳系演化的限制，以及它们与球粒陨石挥发性元素特征的关系。在之前的工作中，母体的 NC 或 CC 特征被用来推断其在原行星盘中的吸积位置。据称 NC 群起源于内盘，而 CC 群则来自外盘，其中盘的 NC 和 CC 区域可能在早期被原木星、压力最大值或尘埃陷阱分开磁盘。所有 CC 母体都在外盘中吸积的原则部分基于证据，即与 NC 陨石相比，少数 CC 陨石富含挥发性物质。在这里，回顾了陨石的挥发性元素和核合成同位素组成是否以及如何与圆盘内的吸积位置相关联。全岩陨石样品的核合成同位素组成与其主要挥发性元素组成（即 C、N 和 O）的趋势形成对比。尽管在比较一些石质 NC 和 CC 陨石及其在盘内推断的吸积位置时，挥发性丰度可能会增加，但这不一定是一般规则。讨论了推断母体吸积位置的困难。发现不能总是假设在 CC 储层中形成的母体相对于在 NC 储层中形成的母体是“富挥发分”的。因此，使用 NC-CC 同位素二分法追踪陆地挥发物的起源仍然具有挑战性。发现不能总是假设在 CC 储层中形成的母体相对于在 NC 储层中形成的母体是“富挥发分”的。因此，使用 NC-CC 同位素二分法追踪陆地挥发物的起源仍然具有挑战性。发现不能总是假设在 CC 储层中形成的母体相对于在 NC 储层中形成的母体是“富挥发分”的。因此，使用 NC-CC 同位素二分法追踪陆地挥发物的起源仍然具有挑战性。