来自Noerdlinger Ries撞击坑的撞击岩的中红外光谱学
Mid-Infrared spectroscopy of impactites from the Noerdlinger Ries impact crater
摘要：
这项研究是为MERTIS（水星辐射计和热红外光谱仪）建立中红外光谱数据库（7- 14微米）的努力的一部分，MERTIS是欧空局/JAXA BepiColombo空间探测器上的一种仪器，将于2017年发射到水星。水星在其历史上曾多次受到撞击。对陆地撞击岩的这项研究可以估计冲击变质作用对行星物质中红外光谱特性的影响。在这项研究中，我们专注于德国南部的Noerdlinger Ries陨石坑，这是一个保存完好且易于进入的撞击坑，拥有丰富的苏埃维特撞击岩。对来自Otting和Aumuehle的Suevite和熔融玻璃块体样品以及来自Polsingen的红色Suevite进行了表征，并获得了它们在中红外范围内的反射光谱。此外，原位中红外光谱由薄切片中的玻璃和基质区域制成。结果表明，类似的，但可区分的光谱散装苏埃维特和熔融玻璃样品，以及在原位测量。来自Aumuehle和Otting的冲击熔融玻璃具有由9.3-9.6微米处的Reststrahlen带主导的光谱。来自Polsingen的大块熔融岩石和大块苏埃维特和细粒基质在9.4至9.6微米之间具有最强的带。还存在与结晶相相关的8.5 - 9微米和12.5 - 12.8微米之间的特征。在细粒基质中有风化产物的证据，如蒙皂石。水星在其历史上经历了各种大小的撞击物的多次撞击。因此，对于像里斯撞击事件那样只在一次撞击中形成的撞击岩所观察到的光谱特征，可以预期在过去遭受过更多撞击的行星体上是非常常见的。我们的结论是，在中红外遥感数据的水星表面可以预期的主要功能的非晶材料。
英文摘要：
This study is part of an effort to build a mid-infrared database (7-14micron) of spectra for MERTIS (Mercury Radiometer and Thermal Infrared Spectrometer), an instrument onboard of the ESA/JAXA BepiColombo space probe to be launched to Mercury in 2017. Mercury was exposed to abundant impacts throughout its history. This study of terrestrial impactites can provide estimates of the effects of shock metamorphism on the mid-infrared spectral properties of planetary materials. In this study, we focus on the Noerdlinger Ries crater in Southern Germany, a well preserved and easily accessible impact crater with abundant suevite impactites. Suevite and melt glass bulk samples from Otting and Aumuehle, as well as red suevite from Polsingen were characterized and their reflectance spectra in mid-infrared range obtained. In addition, in-situ mid-infrared spectra were made from glasses and matrix areas in thin sections. The results show similar, but distinguishable spectra for both bulk suevite and melt glass samples, as well as in-situ measurements. Impact melt glass from Aumuehle and Otting have spectra dominated by a Reststrahlen band at 9.3-9.6 micron. Bulk melt rock from Polsingen and bulk suevite and fine-grained matrix have their strongest band between 9.4 to 9.6 micron. There are also features between 8.5 and 9 micron, and 12.5 - 12.8 micron associated with crystalline phases. There is evidence of weathering products in the fine-grained matrix, such as smectites. Mercury endured many impacts with impactors of all sizes over its history. So spectral characteristics observed for impactites formed only in a single impact like in the Ries impact event can be expected to be very common on planetary bodies exposed to many more impacts in their past. We conclude that in mid-infrared remote sensing data the surface of Mercury can be expected to be dominated by features of amorphous materials.
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