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月球典型撞击坑溅射物研究及对月球地质编图的意义
引用本文:郭弟均,刘建忠,籍进柱,刘敬稳,王庆龙.月球典型撞击坑溅射物研究及对月球地质编图的意义[J].岩石学报,2016,32(1):53-63.
作者姓名:郭弟均  刘建忠  籍进柱  刘敬稳  王庆龙
作者单位:中国科学院地球化学研究所, 月球与行星科学研究中心, 贵阳 550081;中国科学院大学, 北京 100049,中国科学院地球化学研究所, 月球与行星科学研究中心, 贵阳 550081,中国科学院地球化学研究所, 月球与行星科学研究中心, 贵阳 550081;中国科学院大学, 北京 100049,中国科学院地球化学研究所, 月球与行星科学研究中心, 贵阳 550081;中国科学院大学, 北京 100049,吉林大学地球科学学院, 长春 130061
基金项目:本文受国家自然科学基金重大项目(41490634)及面上项目(41373068)、科技基础性工作专项(2015FY210500)和中国科学院知识创新工程重要方向项目联合资助.
摘    要:撞击坑是月表最典型的地质单元,其溅射物作为撞击坑的坑外组成部分可分布到距离坑中心10个直径距离之外的区域,因此撞击溅射物也是月球地质编图中最重要的表达要素之一。本文使用月球勘测轨道器(LRO)的激光高度计(LOLA)数据、广角相机(WAC)影像、窄角相机(NAC)影像以及Clementine的UVVIS多光谱数据,研究了哥白尼纪正面月海区直径31km的Kepler撞击坑和背面月陆区直径30km的Necho撞击坑。哥白尼纪撞击坑溅射沉积物可以分为三个相:连续溅射沉积相(CE)、不连续溅射沉积相(DE)和辐射纹(CR)。连续溅射沉积相分布在最大约2.6个半径范围之内,不连续溅射沉积相分布在最大近11个半径范围之内,辐射纹分布在最大近29个半径范围之内。本文强调了多源数据结合在识别撞击坑溅射沉积物中的作用,对Kepler坑和Necho坑溅射沉积物进行了填图,不对称分布的特征表明这两个坑可能形成于倾斜撞击。

关 键 词:月球  Kepler坑  Necho坑  撞击坑溅射物  辐射纹
收稿时间:2015/6/26 0:00:00
修稿时间:2015/10/11 0:00:00

A study of lunar typical crater ejecta and its implications for lunar geologic mapping
GUO DiJun,LIU JianZhong,JI JinZhu,LIU JingWen and WANG QingLong.A study of lunar typical crater ejecta and its implications for lunar geologic mapping[J].Acta Petrologica Sinica,2016,32(1):53-63.
Authors:GUO DiJun  LIU JianZhong  JI JinZhu  LIU JingWen and WANG QingLong
Institution:Lunar and Planetary Science Research Center, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550081, China;University of Chinese Academy of Sciences, Beijing 100049, China,Lunar and Planetary Science Research Center, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550081, China,Lunar and Planetary Science Research Center, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550081, China;University of Chinese Academy of Sciences, Beijing 100049, China,Lunar and Planetary Science Research Center, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550081, China;University of Chinese Academy of Sciences, Beijing 100049, China and College of Earth Sciences, Jilin University, Changchun 130061, China
Abstract:Crater is the most typical geologic unit on the lunar surface. As the outer part of a crater, the ejecta often occurs even beyond ten crater diameters, which makes it one of the most important features during lunar geologic mapping. By using of the lunar orbiter laser altimeter (LOLA) data, wide-angle camera (WAC) images and narrow-angle camera (NAC) images in Lunar Reconnaissance Orbiter (LRO) mission and Clementine UVVIS multispectral data, we studied the 31km in diameter crater Kepler which locates in the nearside mare region and 30km in diameter crater Necho which locates in the farside land region, both of them belong to Copernican. Copernican crater ejecta can be divided into three faces, which are continuous ejecta deposits (CE), discontinuous ejecta deposits (DE) and crater ray (CR). CE is distributed in a max distance of about 2.6 radii. DE is distributed in a max distance of almost 11 radii, and CR is distributed in a max distance of about 29 radii. This paper stresses the significance of the combination of multi-source data in recognizing the ejecta deposits. Multi-source data are used in mapping the ejecta of crater Kepler and crater Necho. The asymmetric distributions of these two craters' ejecta indicate that they were formed in an oblique impact respectively.
Keywords:Moon  Crater Kepler  Crater Necho  Crater ejecta  Crater ray
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