月球哥白尼纪地层特征与地质演化研究

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

- 1.
  中国地质科学院地质研究所, 北京 100037
- 2.
  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
- 3.
  中国科学院地球化学研究所, 贵阳 550002
- 4.
  中国地质调查局发展研究中心, 北京 100037
- 5.
  民政部卫星减灾应用中心, 北京 100124
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.

收稿日期: 2015-06-08

修回日期: 2015-10-01

刊出日期: 2016-01-31

Study on geological evolution and stratigraphic features of the Copernican Period of the Moon

- 1.
  Institute of Geology, Chinese Academy of Geological Sciences, Beijing 100037, China
- 2.
  Xi'an Aerors Data Technology Co., Ltd, Xi'an 710100, China;Space Star Technology Co., Ltd, Beijing 100038, China
- 3.
  Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550002, China
- 4.
  Development and Research Center, China Geological Survey, Beijing 100037, China
- 5.
  Satellite Disaster Reduction Application Center, Ministry of Civil Affairs, Beijing 100124, China

Received Date: 08 June 2015

Revised Date: 01 October 2015

Publish Date: 31 January 2016

摘要

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(C1)、中哥白尼世地层(C2)和晚哥白尼世地层(C3),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。
- 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
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.

HTML全文

参考文献(47)

[1]	Alexander Jr EC, Bates A, Coscio Jr MR et al. 1976. K/Ar dating of lunar soils. Ⅱ. In: Proceedings of the 7^th Lunar Science Conference. New York: Pergamon Press, 1: 625-648
[2]	Bernatowicz TJ, Hohenberg CM, Hudson B et al. 1978. Argon ages for lunar breccias 14064 and 15405. In: Proceedings of the 9^th Lunar Science Conference. New York: Pergamon Press, 1: 905-919
[3]	Bogard DD, Garrison DH, Shih CY et al. 1994. ³⁹Ar-⁴⁰Ar dating of two lunar granites: The age of copernicus. Geochimica et Cosmochimica Acta, 58(14): 3093-3100
[4]	Claeys P and Morbidelli A. 2011. Late Heavy Bombardment. Berlin Heidelberg: Springer, 909-912
[5]	Deutsch A and Stöffler D. 1987. Rb-Sr-analyses of Apollo 16 melt rocks and a new age estimate for the imbrium basin: Lunar basin chronology and the early heavy bombardment of the moon. Geochimica et Cosmochimica Acta, 51(7): 1951-1964
[6]	Ding XZ, Wang L, Han KY et al. 2014. The lunar digital geological mapping based on ArcGIS: Taking the Arctic Region as an example. Earth Science Frontiers, 21(6): 19-30 (in Chinese with English abstract)
[7]	Dundas CM and McEwen AS. 2007. Rays and secondary craters of Tycho. Icarus, 186(1): 31-40
[8]	Eberhardt P, Geiss J, Grögler N et al. 1973. How old is the crater copernicus? The Moon, 8(1-2): 104-114
[9]	Gomes R, Levison HF, Tsiganis K et al. 2005. Origin of the cataclysmic Late Heavy Bombardment period of the terrestrial planets. Nature, 435(7041): 466-469
[10]	Grier JA, Mcewen AS, Lucey PG et al. 2001. Optical maturity of ejecta from large rayed lunar craters. Journal of Geophysical Research: Planets, 106(E12): 32847-32862
[11]	Guinness EA and Arvidson RE. 1977. On the constancy of the lunar cratering flux over the past 3.3 billion yr. In: Proceedings of the 8^th Lunar Science Conference. New York: Pergamon Press, 3: 3475-3494
[12]	Hartmann WK. 1972. Paleocratering of the moon: Review of post-Apollo data. Astrophysics and Space Science, 17(1): 48-64
[13]	Hartmann WK, Strom RG, Weidenschilling SJ et al. 1981. Chronology of Planetary Volcanism by Comparative Studies of Planetary Cratering. New York: Pergamon Press, 1049-1127
[14]	Hawke BR, Blewett DT, Lucey PG et al. 1999. The composition and origin of selected lunar crater rays. In: New Views of the Moon 2: Understanding the Moon through the Integration of Diverse Datasets. Lunar and Planetary Exploration, 22
[15]	Hawke BR, Blewett DT, Lucey PG et al. 2004. The origin of lunar crater rays. Icarus, 170(1): 1-16
[16]	Head JW and Wilson L. 1992. Lunar mare volcanism: Stratigraphy, eruption conditions, and the evolution of secondary crusts. Geochimica et Cosmochimica Acta, 56(6): 2155-2175
[17]	Jessberger E, Kirsten T and Staudacher T. 1977. One rock and many ages: Further K-Ar dat on consortium breccia 73215. In: Proceedings of the 8^th Lunar Science Conference. New York: Pergamon Press, 2567-2580
[18]	Jolliff BL, Wieczorek MA, Shearer CK et al. 2006. New Views of the Moon. Chantilly, Virginia: Mineralogical Society of America
[19]	Lucey PG, Blewett DT, Taylor GJ et al. 2000. Imaging of lunar surface maturity. Journal of Geophysical Research: Planets, 105(E8): 20377-20386
[20]	Meyer Jr C, Brett R, Hubbard NJ et al. 1971. Mineralogy, chemistry, and origin of the kreep component in soil samples from the ocean of storms. In: Proceedings of the 2^nd Lunar Science Conference. New York: Pergamon Press, 393-411
[21]	Nakamura Y, Lammlein D, Latham G et al. 1973. New seismic data on the state of the deep lunar interior. Science, 181(4094): 49-51
[22]	Neukum G and König B. 1976. Dating of individual lunar craters. In: Proceedings of the 7^th Lunar Science Conference. New York: Pergamon Press, 2867-2881
[23]	Neukum G and Ivanov BA. 1994. Crater size distributions and impact probabilities on earth from lunar, terrestrial-planet and asteroid cratering data. In: Hazard due to Comets and Asteroids. Tucson, Arizona: University of Arizona Press, 359-416
[24]	Ouyang ZY. 2005. Introduction to Lunar Science. Beijing: China Aerospace Press, 1-362 (in Chinese)
[25]	Ryder G and Spudis P. 1987. Chemical composition and origin of apollo 15 impact melts. Journal of Geophysical Research: Solid Earth, 92(B4): E432-E446
[26]	Ryder G, Bogard D and Garrison D. 1991. Probable age of autolycus and calibration of lunar stratigraphy. Geology, 19: 143-146
[27]	Shoemaker EM and Hackman RJ. 1962. Stratigraphic basis for a lunar time scale. In: In the Moon: Proceedings of Symposium No.14 of the International Astronomical Union, Leningrad, 1960. New York: Academic Press, 289-300
[28]	Silver LT. 1971. U-Th-Pb isotope in Apollo 11 and Apollo 12 regolithic materials and a possible Copernicus impact event. Transactions American Geophysical Union, 52: 534
[29]	Soderblom LA, Boyce JM, Arnold JR et al. 1977. Regional variations in the lunar maria-age, remanent magnetism, and chemistry. In: Proceedings of the 8^th Lunar Science Conference. New York: Pergamon Press, 1: 1191-1199
[30]	Stadermann FJ, Heusser E, Jessberger EK et al. 1991. The case for a younger imbrium basin: ⁴⁰Ar-³⁹Ar ages of Apollo 14 rocks. Geochimica et Cosmochimica Acta, 55(8): 2339-2349
[31]	Stöffler D, Bischoff A, Borchardt R et al. 1985. Composition and evolution of the lunar crust in the descartes highlands, Apollo 16. Journal of Geophysical Research: Solid Earth, 90(S02): C449-C506
[32]	Stöffler D and Ryder G. 2001. Stratigraphy and isotope ages of lunar geologic units: Chronological standard for the inner solar system. Space Science Reviews, 96(1-4): 9-54
[33]	Stöffler D, Ryder G, Ivanov BA et al. 2006. Cratering history and lunar chronology. Reviews in Mineralogy and Geochemistry, 60(1): 519-596
[34]	Turcotte DL and Schubert G. 1982. Geodynamics: Application of Continuum Physics to Geological Problems. New York: Cambridge University Press
[35]	Wang L, Ding XZ, Han TL et al. 2015. The digital geological mapping and geological and geomorphic features of Tycho crater of the Moon. Earth Science Frontiers, 22(2): 251-262 (in Chinese with English abstract)
[36]	Wilhelms DE. 1970. Summary of Lunar Stratigraphy: Telescopic Observations. Washington DC: US Government Printing Office
[37]	Wilhelms DE, McCauley JF and Trask NJ. 1987. The Geologic History of the Moon. Washington DC: US Government Printing Office
[38]	Xiao L, Zhu P, Fang G et al. 2015. A young multilayered terrane of the northern Mare Imbrium revealed by Chang'E-3 mission. Science, 347(6227): 1226-1229
[39]	Xiao ZY. 2013. Comparison between Copernican-aged geological activity on the moon and Kuiperian-aged geological activity on mercury. Ph. D. Dissertation. Beijing: China University of Geosciences, 62-88 (in Chinese)
[40]	Xiao ZY, Zeng ZX, Xiao L et al. 2013. The small stretch and compressional tectonics on continuous sputtering blanket of the Copernicus crater of the Moon: A global contraction and the local stress counter. Geological Journal of China Universities, 19(Suppl.): 626(in Chinese)
[41]	Young RA. 1977. The lunar impact flux, radiometric age correlation, and dating of specific lunar features. In: Proceedings of the 8^th Lunar Science Conference. New York: Pergamon Press, 3457-3473
[42]	Zhang J, Yang W, Hu S et al. 2015. Volcanic history of the Imbrium basin: A close-up view from the lunar rover Yutu. Proceedings of the National Academy of Sciences of the United States of America, 112(17): 5342-5347
[43]	丁孝忠, 王梁, 韩坤英等. 2014. 基于ArcGIS的月球数字地质填图: 以月球北极地区为例. 地学前缘, 21(6): 19-30
[44]	欧阳自远. 2005. 月球科学概论. 北京: 中国宇航出版社, 1-362
[45]	王梁, 丁孝忠, 韩同林等. 2015. 月球第谷撞击坑区域数字地质填图及地质地貌特征. 地学前缘, 22(2): 251-262
[46]	肖智勇. 2013. 月球表面哥白尼纪与水星表面柯伊伯纪的地质活动对比研究. 博士学位论文. 北京: 中国地质大学, 62-88
[47]	肖智勇, 曾佐勋, 肖龙等. 2013. 月球哥白尼撞击坑连续溅射毯上的小型拉伸与挤压构造: 全球收缩与局部应力的抗衡. 高校地质学报, 19(增刊): 626

施引文献

资源附件(0)

访问统计

点击查看大图

计量

文章访问数: 6390
PDF下载数: 7302
施引文献: 0

月球哥白尼纪地层特征与地质演化研究

Study on geological evolution and stratigraphic features of the Copernican Period of the Moon

计量

出版历程

目录