| 月球哥白尼纪地层特征与地质演化研究 |
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| 引用本文： | 丁孝忠,王梁,郭弟均,王翔,韩坤英,庞健峰,王丹,陶亮.月球哥白尼纪地层特征与地质演化研究[J].岩石学报,2016,32(1):10-18. |
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| 作者姓名： | 丁孝忠 王梁 郭弟均 王翔 韩坤英 庞健峰 王丹 陶亮 |
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| 作者单位： | 中国地质科学院地质研究所, 北京 100037,西安航天天绘数据技术有限公司, 西安 710100;航天恒星科技有限公司, 北京 100038,中国科学院地球化学研究所, 贵阳 550002,中国地质调查局发展研究中心, 北京 100037,中国地质科学院地质研究所, 北京 100037,中国地质科学院地质研究所, 北京 100037,中国地质科学院地质研究所, 北京 100037,民政部卫星减灾应用中心, 北京 100124 |
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| 基金项目： | 本文受科技部科技基础性工作专项(2015FY210500)、国家高技术研究发展计划"863"项目(2009AA122201)、国家自然科学基金重大项目(41490634)、中国科学院地球化学研究所领域前沿项目(Y2ZZ031000-02)、国家重大科技专项"高分辨率对地观测系统"和民用航天十二五预研项目联合资助. |
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| 摘 要： | 月球哥白尼纪地层是月球演化历史中最年轻的地层单元,哥白尼纪撞击坑数量较少,但其形成的哥白尼纪地层却是全球性的、非常显著的,大多学者普遍认为哥白尼纪基本没有岩浆活动与构造活动。通过对月球哥白尼纪地层进行地质填图,认为月球高地地区撞击坑辐射纹相对月海地区辐射纹发育更好,推测其原因可能为高地与月海岩石性质不同,或撞击的小天体体积、能量、物质特征以及撞击的角度、速度不同等原因导致的;哥白尼纪地层可划分为早哥白尼世地层(C_1)、中哥白尼世地层(C_2)和晚哥白尼世地层(C_3),通过对各世典型撞击坑的分析与研究,阐述了哥白尼纪各世地层的特征,为开展月球晚期撞击作用特征与效应的研究提供了资料。对哥白尼纪-爱拉托逊纪地层界限进行了初步探讨,提出月球年代学多源数据综合判别法方案,以重新厘定哥白尼纪年代下限。
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| 关 键 词： | 月球哥白尼纪地层特征 哥白尼纪地层划分 地质演化 哥白尼纪-爱拉托逊纪界限 |
| 收稿时间： | 6/8/2015 12:00:00 AM |
| 修稿时间： | 2015/10/1 0:00:00 |
Study on geological evolution and stratigraphic features of the Copernican Period of the Moon |
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| DING XiaoZhong,WANG Liang,GUO DiJun,WANG Xiang,HAN KunYing,PANG JianFeng,WANG Dan and TAO Liang.Study on geological evolution and stratigraphic features of the Copernican Period of the Moon[J].Acta Petrologica Sinica,2016,32(1):10-18. |
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| Authors: | DING XiaoZhong WANG Liang GUO DiJun WANG Xiang HAN KunYing PANG JianFeng WANG Dan and TAO Liang |
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| Institution: | Institute of Geology, Chinese Academy of Geological Sciences, Beijing 100037, China,Xi'an Aerors Data Technology Co., Ltd, Xi'an 710100, China;Space Star Technology Co., Ltd, Beijing 100038, China,Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550002, China,Development and Research Center, China Geological Survey, Beijing 100037, China,Institute of Geology, Chinese Academy of Geological Sciences, Beijing 100037, China,Institute of Geology, Chinese Academy of Geological Sciences, Beijing 100037, China,Institute of Geology, Chinese Academy of Geological Sciences, Beijing 100037, China and Satellite Disaster Reduction Application Center, Ministry of Civil Affairs, Beijing 100124, China |
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| Abstract: | The Copernican strata is the youngest stratigraphic units of the evolutionary history of the Moon. A few impact craters formed in Copernican Period, but the Copernican strata formed by them are indeed global and very significant. Most scholars generally believed that there are no magmatism and tectonic activity basically in the Copernican Period. The radiation pattern of the craters in highlands is relatively better development than which on the mare area through the study of geological mapping of Copernican strata of the Moon, the reason may be the rocks on highlands or on the mare are different in nature, and the size, energy, material characteristics of small objects and the different angles of the impact, and so on. The strata of Copernican Period can be divided into Early Copernican Series (C1), Middle Copernican Series (C2) and Late Copernican Series (C3). This paper explained the stratigraphic characteristics of each epoch of Copernican Period through the analyzing and studying on the typical impact craters, which provided the information for the features and effects of the younger impact action of the Moon. Finally, this paper discussed the stratigraphic boundary of Copernican Period-Eratosthenian Period briefly, and proposed a new program by integration discrimination based on lunar chronology multi-source data to re-determine the lower limit of Copernican Period. |
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| Keywords: | Stratigraphic features of the Copernican Period of the Moon Division of the Copernican Period Tectonic evolution Stratigraphic boundary of Copernican Period-Eratosthenian Period |
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