IIE铁与普通、F和HH球粒陨石之间关系的统计研究

IF 2.4 4区 地球科学 Q2 GEOCHEMISTRY & GEOPHYSICS
Rachel S. Kirby, Penelope L. King, Andrew G. Tomkins
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引用次数: 0

摘要

有人提出,IIE铁陨石是由H球粒陨石或备受争议的第四种普通球粒陨石HH球粒陨石组成的母体撞击形成的。为了解决这一争论,我们编制了普通球粒陨石、低球粒陨石未分组球粒陨石和IIE铁的大型数据集,并进行了统计分析,以确定:(1)目前普通球粒陨石组的分类在统计上是否合适;(2) IIE铁与H球粒陨石有关,或者它们是否代表了在“HH”球粒陨石母体上形成的不同群。研究表明,目前基于岩石学、橄榄石和正辉石化学的分类体系适合于H、L和LL球粒陨石。我们定义了第四个“F球粒陨石”组,由8个以前未分组的非常低fa的3型和4型球粒陨石组成。单靠Δ17O数据的统计分析无法区分H型球粒陨石和IIE铁,也无法区分L型和LL型球粒陨石。此外,统计分析无法在所有测量(矿物化学、球粒大小、体积Δ17O、Ge和Mo同位素组成以及金属中亲铁元素的体积丰度)中区分H球粒陨石和IIE铁;没有证据表明存在“HH”球粒陨石群。这些结果与在H球粒陨石母体上通过撞击熔融和近表面金属偏析形成IIE铁陨石的理论一致。H球粒陨石和IIE铁之间的遗传联系使我们能够了解行星形成和演化过程中发生的地球化学和岩石学变化。
本文章由计算机程序翻译,如有差异,请以英文原文为准。

A statistical investigation into relationships between the IIE irons and the ordinary, F and “HH” chondrites

A statistical investigation into relationships between the IIE irons and the ordinary, F and “HH” chondrites

It has been proposed that IIE iron meteorites formed through impact processes on a parent body that was composed of either the H chondrites or a much-debated fourth ordinary chondrite group, the HH chondrites. To resolve this debate, we have compiled a large dataset for the ordinary chondrites, low-fayalite ungrouped chondrites, and IIE irons, and undertaken a statistical analysis to determine if: (1) the current classification of ordinary chondrite groups is statistically appropriate; and (2) the IIE irons are related to H chondrites or if they represent a distinct group that formed on a “HH” chondrite parent body. We demonstrate that the current classification system based on petrography and olivine and orthopyroxene chemistry is appropriate for the H, L, and LL chondrites. We define a fourth “F chondrite” group consisting of eight, previously ungrouped, very low-Fa Type 3 and 4 chondrites. Statistical analysis of Δ17O data alone cannot distinguish between the H chondrites and IIE irons, nor between the L and LL chondrites. Furthermore, statistical analyses are unable to distinguish H chondrites from IIE irons in all measures (mineral chemistry, chondrule size, bulk Δ17O, Ge and Mo isotopic compositions, and bulk siderophile element abundances in metal); there is no evidence for a “HH” chondrite group. These results are consistent with formation of IIE iron meteorites through impact melting and near-surface metal segregation on the H chondrite parent body. This genetic link between H chondrites and IIE irons allows us to understand the geochemical and petrological changes that occurred during planetary formation and evolution.

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来源期刊
Meteoritics & Planetary Science
Meteoritics & Planetary Science 地学天文-地球化学与地球物理
CiteScore
3.90
自引率
31.80%
发文量
121
审稿时长
3 months
期刊介绍: First issued in 1953, the journal publishes research articles describing the latest results of new studies, invited reviews of major topics in planetary science, editorials on issues of current interest in the field, and book reviews. The publications are original, not considered for publication elsewhere, and undergo peer-review. The topics include the origin and history of the solar system, planets and natural satellites, interplanetary dust and interstellar medium, lunar samples, meteors, and meteorites, asteroids, comets, craters, and tektites. Our authors and editors are professional scientists representing numerous disciplines, including astronomy, astrophysics, physics, geophysics, chemistry, isotope geochemistry, mineralogy, earth science, geology, and biology. MAPS has subscribers in over 40 countries. Fifty percent of MAPS'' readers are based outside the USA. The journal is available in hard copy and online.
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