S. A. Eckley, R. A. Ketcham, Y. Liu, J. Gross, F. M. McCubbin
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引用次数: 0
摘要
谢尔戈特岩是黑云母至超黑云母火成岩,占已知火星陨石的大多数。根据矿物学和质地的不同,它们又被细分为辉长岩、辉绿岩、玄武岩和橄榄斑岩等类别。这些陨石的地质环境尚不清楚,因此通常使用晶体大小和偏好方向的分析来推断舍尔格特石的凝固地点。这些环境包括地表下的积岩、浅侵入岩和喷出熔岩流,它们对与地壳物质的相互作用、冷却历史和地表的潜在原位暴露都有不同的影响。在这项研究中,我们提出了一种新颖的三维(3-D)方法,以更好地了解这些样品的凝固环境,并增进我们对舍尔格特岩地质背景的了解。我们使用 X 射线计算机断层扫描(CT)技术,对代表辉长岩、辉绿岩、玄武岩和橄榄斑岩类别的八种谢尔戈特岩进行了三维测量,结果显示大多数相的形状优先取向和后期形成矿物的晶体尺寸分布。我们的分析表明,在辉长岩样品中,高度各向异性的棒状辉石晶体具有强烈的褶皱,但在玄武岩样品中,褶皱较弱,线纹较轻,这表明后者中存在定向流动成分。星体体积分布分析表明,大多数相(蒙德拉石、辉石、橄榄石和氧化物/硫化物)都保留了强度不等的褶皱纹理,而且各个样品中的相彼此间的排列从强烈到适度不等。结合根据间隙氧化物/硫化物晶体尺寸分布分析确定的结晶最后阶段的相对冷却率,这些结果表明橄榄石斑岩样品是作为浅侵入体(如尖晶石/闪长岩)堆积的,而辉长岩、辉绿岩和玄武岩样品是在较深的地下环境中堆积的。
Emplacement of shergottites in the Martian crust inferred from three-dimensional petrofabric and crystal size distribution analyses
Shergottites are mafic to ultramafic igneous rocks that represent the majority of known Martian meteorites. They are subdivided into gabbroic, poikilitic, basaltic, and olivine–phyric categories based on differences in mineralogy and textures. Their geologic contexts are unknown, so analyses of crystal sizes and preferred orientations have commonly been used to infer where shergottites solidified. Such environments range from subsurface cumulates to shallow intrusives to extrusive lava flows, which all have contrasting implications for interactions with crustal material, cooling histories, and potential in situ exposure at the surface. In this study, we present a novel three-dimensional (3-D) approach to better understand the solidification environments of these samples and improve our knowledge of shergottites' geologic contexts. Shape preferred orientations of most phases and crystal size distributions of late-forming minerals were measured in 3-D using X-ray computed tomography (CT) on eight shergottites representing the gabbroic, poikilitic, basaltic, and olivine–phyric categories. Our analyses show that highly anisotropic, rod-like pyroxene crystals are strongly foliated in the gabbroic samples but have a weaker foliation and a mild lineation in the basaltic sample, indicating a directional flow component in the latter. Star volume distribution analyses revealed that most phases (maskelynite, pyroxene, olivine, and oxides/sulfides) preserve a foliated texture with variable strengths, and that the phases within individual samples are strongly to moderately aligned with respect to one another. In combination with relative cooling rates during the final stages of crystallization determined from interstitial oxide/sulfide crystal size distribution analyses, these results indicate that the olivine–phyric samples were emplaced as shallow intrusives (e.g., dikes/sills) and that the gabbroic, poikilitic, and basaltic samples were emplaced in deeper subsurface environments.
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.