Elmshorn(H3-6)的异常多晶普通软玉角砾岩--可能在大约2.8亿年前,两个普通软玉母体发生碰撞、完全破坏和混合后的晚期再生成物

IF 2.2 4区 地球科学 Q2 GEOCHEMISTRY & GEOPHYSICS
Addi Bischoff, Markus Patzek, Romain M. L. Alosius, Jean-Alix Barrat, Jasper Berndt, Henner Busemann, Detlev Degering, Tommaso Di Rocco, Mattias Ek, Jérôme Gattacceca, Jose R. A. Godinho, Dieter Heinlein, Daniela Krietsch, Colin Maden, Oscar Marchhart, Martin Martschini, Silke Merchel, Andreas Pack, Stefan Peters, Miriam Rüfenacht, Jochen Schlüter, Maria Schönbächler, Aleksandra Stojic, Jakob Storz, Wolfgang Tillmann, Alexander Wieser, Karl Wimmer, Reiner Zielke
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引用次数: 0

摘要

Elmshorn 于 2023 年 4 月 25 日坠落在德国汉堡市西北约 30 公里处。坠落后不久,人们找到了 21 块碎片,总重 4277 克。Elmshorn 是一种多晶体和异常 H3-6 刚玉碎屑角砾岩。岩石由典型的 H 型软玉岩岩性和中等 H/L 型(或 L 型,基于磁性)软玉岩来源的碎屑混合而成。在这 21 块岩石中,有些以 H 型闪长岩岩性为主,有些则以 H/L 型(或 L 型)闪长岩成分为主。这些成分的H/L雪龙岩归属是基于平衡4型碎片(~Fa21-22)中橄榄石的平均成分。密度(3.34 g cm-3)和磁感应强度(logχ <5.0,χ 单位为 10-9 m3 kg-1)等物理性质是典型的 L 型雪龙岩,这与氧同位素组成不一致:来自两个不同碎片的所有八种 O 同位素分析结果都明显属于 H 型雪龙岩。因此,在散布区发现的碎片在矿物学、矿物化学和物理性质方面各不相同,但在 O 同位素特征方面却不尽相同。研究最深入的样本属于以 H chondrite 岩石为主的石头。化学成分以及核合成 Cr 和 Ti 同位素数据是普通软玉的典型特征。Elmshorn 中的惰性气体是宇宙生成惰性气体、放射生成惰性气体和原始惰性气体的混合物,同时可以排除太阳风成分。由于埃尔姆索恩的软玉质岩石包含(a)H 型软玉母体内部物质(第 5 和第 6 类),(b)软玉母体近表面物质(第 3 和第 4 类),(c)H/L 型软玉的碎片(在许多石头中占主导地位),(d)冲击变暗的碎片,以及(e)各种撞击熔融物的碎屑,但没有太阳风植入的惰性气体,因此不同的成分不可能是母体碎屑的一部分。最直截了当的解释是,Elmshorn 的碎屑角砾岩是一个 H 型软玉母体与另一个具有 H/L 型(或 L 型)软玉特征但 O 同位素值(即 H 型软玉的 O 同位素值)不同的母体发生灾难性碰撞、母体完全破碎、混合和重新组合后重新生成的岩石。这是避免太阳风气体植入这种复杂角砾岩的唯一直接方法。约 2.8 Gyr 的气体滞留年龄可能表明了 H 型和 H/L 型(或 L 型)软玉母体发生灾难性碰撞后的闭合时间,而 Elmshorn 的宇宙射线暴露年龄约为 17-20 Myr,其大气层前半径为 25-40 cm。
本文章由计算机程序翻译,如有差异,请以英文原文为准。

The anomalous polymict ordinary chondrite breccia of Elmshorn (H3-6)—Late reaccretion after collision between two ordinary chondrite parent bodies, complete disruption, and mixing possibly about 2.8 Gyr ago

The anomalous polymict ordinary chondrite breccia of Elmshorn (H3-6)—Late reaccretion after collision between two ordinary chondrite parent bodies, complete disruption, and mixing possibly about 2.8 Gyr ago

Elmshorn fell April 25, 2023, about 30 km northwest of the city of Hamburg (Germany). Shortly after the fall, 21 pieces were recovered totaling a mass of 4277 g. Elmshorn is a polymict and anomalous H3-6 chondritic, fragmental breccia. The rock is a mixture of typical H chondrite lithologies and clasts of intermediate H/L (or L, based on magnetic properties) chondrite origin. In some of the 21 pieces, the H chondrite lithologies dominate, while in others the H/L (or L) chondrite components are prevalent. The H/L chondrite assignment of these components is based on the mean composition of their olivines in equilibrated type 4 fragments (~Fa21–22). The physical properties like density (3.34 g cm−3) and magnetic susceptibility (logχ <5.0, with χ in 10−9 m3 kg−1) are typical for L chondrites, which is inconsistent with the oxygen isotope compositions: all eight O isotope analyses from two different fragments clearly fall into the H chondrite field. Thus, the fragments found in the strewn field vary in mineralogy, mineral chemistry, and physical properties but not in O isotope characteristics. The sample most intensively studied belongs to the stones dominated by H chondrite lithologies. The chemical composition and nucleosynthetic Cr and Ti isotope data are typical for ordinary chondrites. The noble gases in Elmshorn represent a mixture between cosmogenic, radiogenic, and primordially trapped noble gases, while a solar wind component can be excluded. Because the chondritic rock of Elmshorn contains (a) H chondrite parent body interior materials (of types 5 and 6), (b) chondrite parent body near-surface materials (of types 3 and 4), (c) fragments of an H/L chondrite (dominant in many stones), (d) shock-darkened fragments, and (e) clasts of various types of impact melts but no solar wind-implanted noble gases, the different components cannot have been part of a parent body regolith. The most straightforward explanation is that the fragmental breccia of Elmshorn represents a reaccreted rock after a catastrophic collision between an H chondrite parent body and another body with H/L (or L) chondrite characteristics but with deviating O isotope values (i.e. that of H chondrites), complete disruption of the bodies, mixing, and reassembly. This is the only straightforward way that the implantation of solar wind gases could have been avoided in this kind of complex breccia. The gas retention ages of about 2.8 Gyr possibly indicate the closure time after the catastrophic collision between H and H/L (or L) chondrite parent bodies, while the cosmic ray exposure age for Elmshorn, which had a preatmospheric radius of 25–40 cm, is ~17–20 Myr.

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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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