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首页> 外文期刊>Journal of Volcanology and Geothermal Research >Igneous rocks formed by hypervelocity impact
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Igneous rocks formed by hypervelocity impact

机译：超高速撞击形成的火成岩

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摘要

Igneous rocks are the primary building blocks of planetary crusts. Most igneous rocks originate via decompression melting and/or wet melting of protolith lithologies within planetary interiors and their classification and compositional, petrographic, and textural characteristics, are well-studied. As our exploration of the Solar System continues, so too does the inventory of intrusive and extrusive igneous rocks, settings, and processes. The results of planetary exploration have also clearly demonstrated that impact cratering is a ubiquitous geological process that has affected, and will continue to affect, all planetary objects with a solid surface, whether that be rock or ice. It is now recognized that the production of igneous rocks is a fundamental outcome of hypervelocity impact. The goal of this review is to provide an up-to-date synthesis of our knowledge and understanding of igneous rocks formed by hypervelocity impact. Following a brief overview of the basics of the impact process, we describe how and why melts are generated during impact events and how impact melting differs from endogenic igneous processes. While the process may differ, we show that the products of hypervelocity impact can share close similarities with volcanic and shallow intrusive igneous rocks of endogenic origin. Such impact melt rocks, as they are termed, can display lobate margins and cooling cracks, columnar joints and at the hand specimen and microscopic scale, such rocks can display mineral textures that are typical of volcanic rocks, such as quench crystallites, ophitic, porphyritic, as well as features such as vesicles, flow textures, and soon. Historically, these similarities led to the misidentification of some igneous rocks now known to be impact melt rocks as being of endogenic origin. This raises the question as to how to distinguish between an impact versus an endogenic origin for igneous-like rocks on other planetary bodies where fieldwork and sample analysis may not be possible and all that may be available is remote sensing data. While the interpretation of some impact melt rocks may be relatively straightforward (e.g., for clast-rich varieties and those with clear projectile contamination) we conclude that distinguishing between impact and endogenic igneous rocks is a non-trivial task that ultimately may require sample investigation and analysis to be conducted. Caution is, therefore, urged in the interpretation of igneous rocks on planetary surfaces. (C) 2018 Elsevier B.V. All rights reserved.
机译：火成岩是行星地壳的主要构造块。大多数火成岩是通过行星内部内部原岩岩性的减压融化和/或湿融化而产生的，并且对其分类和成分，岩石学和质地特征进行了深入研究。随着我们对太阳系的探索继续，侵入性和挤压性火成岩，环境和过程的清单也不断增加。行星探测的结果也清楚地表明，撞击坑是一个普遍存在的地质过程，已经影响并将继续影响所有具有固体表面的行星物体，无论是岩石还是冰。现在已经认识到，火成岩的产生是超高速撞击的基本结果。这篇综述的目的是提供我们对由超高速撞击形成的火成岩的知识和理解的最新综合。在简要介绍了冲击过程的基础知识之后，我们描述了在冲击事件期间如何以及为什么产生熔体，以及冲击熔体与内生火成岩过程有何不同。虽然过程可能有所不同，但我们表明，超高速撞击的产物可以与内生成因的火山岩和浅侵入性火成岩有着相似的相似性。这种所谓的冲击熔岩可以显示出叶状边缘和冷却裂缝，柱状接缝，并且在手部样品和微观尺度上可以显示出火山岩所特有的矿物质地，例如淬火微晶，辉光岩，斑状岩，以及小泡，流动纹理等特性。从历史上看，这些相似之处导致对某些火成岩的误判，这些火成岩现在已知是内源性撞击熔岩。这就提出了一个问题，即如何区分其他行星体上火成岩类岩石的撞击与内生起源之间的关系，在这些行星体上可能无法进行实地调查和样品分析，而所有可用的都是遥感数据。尽管某些冲击熔岩的解释可能相对简单（例如，对于含丰富碎屑的品种和具有明显弹丸污染的岩石），但我们得出的结论是，区分冲击岩和内生火成岩是一项艰巨的任务，最终可能需要进行样品调查和进行分析。因此，在解释行星表面火成岩时应格外小心。 （C）2018 Elsevier B.V.保留所有权利。

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    Osinski Gordon R.; Grieve Richard A. F.; Bleacher Jacob E.; Neish Catherine D.; Pilles Eric A.; Tornabene Livio L.;

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    Univ Western Ontario, Dept Earth Sci, Ctr Planetary Sci & Explorat, 1151 Richmond St, London, ON N6A 5B7, Canada;

    Univ Western Ontario, Dept Earth Sci, Ctr Planetary Sci & Explorat, 1151 Richmond St, London, ON N6A 5B7, Canada;

    NASA, Goddard Space Flight Ctr, Geophys & Geochem Lab, Planetary Geol, Code 698, Greenbelt, MD 20771 USA;

    Univ Western Ontario, Dept Earth Sci, Ctr Planetary Sci & Explorat, 1151 Richmond St, London, ON N6A 5B7, Canada;

    Univ Western Ontario, Dept Earth Sci, Ctr Planetary Sci & Explorat, 1151 Richmond St, London, ON N6A 5B7, Canada;

    Univ Western Ontario, Dept Earth Sci, Ctr Planetary Sci & Explorat, 1151 Richmond St, London, ON N6A 5B7, Canada;

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