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首页> 外文期刊>Planetary and space science >Shallow crustal composition of Mercury as revealed by spectral properties and geological units of two impact craters
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Shallow crustal composition of Mercury as revealed by spectral properties and geological units of two impact craters

机译：通过两个撞击坑的光谱特性和地质单位揭示出水星的浅层地壳组成

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We have performed a combined geological and spectral analysis of two impact craters on Mercury: the 15 km diameter Waters crater (106 degrees W; 9 degrees S) and the 62.3 km diameter Kuiper crater (30 degrees W; 11 degrees S). Using the Mercury Dual Imaging System (MDIS) Narrow Angle Camera (NAC) dataset we defined and mapped several units for each crater and for an external reference area far from any impact related deposits. For each of these units we extracted all spectra from the MESSENGER Atmosphere and Surface Composition Spectrometer (MASCS) Visible-InfraRed Spectrograph (VIRS) applying a first order photometric correction. For all the mapped units, we analyzed the spectral slope in two wavelength ranges, 350-450 nm and 450-650 nm, and the absolute reflectance in the 700-750 nm range. Normalized spectra of Waters crater display a generally bluer spectral slope than the external reference area over both wavelength windows. Normalized spectra of Kuiper crater generally display a redder slope than the external reference area in the 350-450 nm window, while they display a bluer slope than the external reference area in the 450-650 nm wavelength range. The combined use of geological and spectral analyses enables reconstruction of the local scale stratigraphy beneath the two craters, providing insight into the properties of the shallower crust of Mercury. Kuiper crater, being similar to 4 times larger than Waters crater, exposes deeper layers with distinctive composition, while the result for Waters crater might indicate substantial compositional homogeneity with the surrounding intercrater plains, though we cannot exclude the occurrence of horizontal compositional heterogeneities in the shallow sub-surface. (C) 2015 Elsevier Ltd. All rights reserved.
机译：我们对水星上的两个撞击坑进行了地质和光谱的组合分析：直径为15公里的沃特斯火山口（106度； 9度南）和直径为62.3公里的柯伊珀火山口（30度；南纬11度）。使用水星双成像系统（MDIS）窄角相机（NAC）数据集，我们为每个火山口和外部参考区域定义并绘制了多个单元，这些单元远离任何与撞击相关的沉积物。对于这些单元中的每一个，我们均采用一阶光度校正从MESSENGER大气和表面成分光谱仪（MASCS）可见红外光谱仪（VIRS）中提取所有光谱。对于所有映射的单位，我们分析了两个波长范围（350-450 nm和450-650 nm）中的光谱斜率，以及700-750 nm范围中的绝对反射率。在两个波长窗口上，沃特斯火山口的归一化光谱显示的光谱斜率通常比外部参考区域要蓝。 Kuiper火山口的归一化光谱通常在350-450 nm窗口中显示出比外部参考区域更红的斜率，而在450-650 nm波长范围中显示出比外部参考区域更蓝的斜率。地质和光谱分析的结合使用，可以重建两个陨石坑下方的局部尺度地层，从而深入了解水星浅层地壳的特性。 Kuiper火山口大约是Waters火山口的4倍，它暴露出具有独特成分的更深层，而Waters火山口的结果可能表明与周围的火山口平原具有相当大的成分同质性，尽管我们不能排除在浅层中存在水平成分异质性次表面。 （C）2015 Elsevier Ltd.保留所有权利。

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