Abstract The study of chondritic meteorites and their components allows us to understand processes and conditions in the protoplanetary disk. Chondrites with high and about equal proportions of chondrules and matrix are ideal candidates to not only study the formation conditions of chondrules, but also the relationship between these two major components. An important question is whether these formed in the same or in separate reservoirs in the protoplanetary disk. So far, such studies have been mainly restricted to carbonaceous chondrites. We here expand these studies to the K (Kakangari-like) chondrite grouplet. These have various distinctive properties, but the abundance of major components – chondrules and matrix – is similar to other primitive meteorites. We obtained a comprehensive petrographic and chemical dataset of Kakangari and Lewis Cliff 87232 chondrules and matrix. Chondrules in Kakangari show a large compositional scatter, supporting material addition to chondrules during their formation. Contrary to almost all other chondrite groups, the majority of Kakangari chondrules are not mineralogically zoned. However, Kakangari chondrules were likely initially zoned, but then lost this zonation during chondrule remelting and fragmentation. Average compositions of bulk chondrules, matrix and bulk Kakangari are identical and approximately solar for Mg/Si. This might indicate the formation of chondrules and matrix from a common reservoir and would agree with findings from carbonaceous and Rumuruti chondrites: chondrules and matrix in most chondrite groups were not transported through the protoplanetary disk and then mixed together. Rather, these major components are genetically related to each other and formed in the same reservoir.

中文翻译：

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卡坎加里球粒陨石中球粒和基质的形成

摘要 球粒陨石及其成分的研究使我们能够了解原行星盘中的过程和条件。球粒陨石和基体比例高且几乎相等的球粒陨石是理想的候选物，不仅可以研究球粒的形成条件，还可以研究这两种主要成分之间的关​​系。一个重要的问题是这些是在原行星盘的相同或不同的水库中形成的。迄今为止，此类研究主要限于碳质球粒陨石。我们在这里将这些研究扩展到 K（Kakangari-like）球粒陨石群。它们具有各种独特的特性，但主要成分——球粒和基质——的丰富程度与其他原始陨石相似。我们获得了 Kakangari 和 Lewis Cliff 87232 球粒和基质的综合岩相和化学数据集。卡坎加里的球粒显示出很大的成分散布，支持在其形成过程中添加到球粒中的物质。与几乎所有其他球粒陨石群相反，大多数卡坎加里球粒在矿物学上没有分带。然而，Kakangari 球粒最初很可能被分带，但在球粒重熔和破碎过程中失去了这种分带。对于 Mg/Si，块状球粒、基质和块状 Kakangari 的平均成分是相同的并且近似于太阳。这可能表明球粒和基质的形成来自一个共同的储层，并且与碳质和 Rumuruti 球粒陨石的发现一致：大多数球粒陨石群中的球粒和基质没有通过原行星盘运输，然后混合在一起。相反，这些主要成分在遗传上彼此相关并形成于同一储层中。