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月球阿波罗盆地区域月壳结构及光谱特征
郭弟均1,2,3, 刘建忠1, HEAD W. James3, 李帅4, POTTERW.K.Ross3, 林红磊2,5
1.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 550002;2.中国科学院大学, 北京 100014;3.Department of Earth, Environmental and Planetary Sciences, Brown University, Providence 02912;4.University of Hawaii at Manoa, Honolulu, HI 96822;5.中国科学院 遥感与数字地球研究所, 北京 100101
摘要:
位于月球南极-艾肯(South Pole-Aitken Basin,SPA)盆地内的前酒海纪阿波罗盆地跨越了SPA盆地的瞬时穴和盆缘。SPA盆地是已确认的月球上最大最古老的撞击盆地,因此阿波罗盆地对于认识月球的内部结构和成分、区域地质作用和演化历史具有不可替代的作用。阿波罗盆地区域月壳具有很强的不对称性,靠近SPA盆缘处厚而靠近SPA盆地中心处薄,其峰环内部拥有最薄的月壳厚度。阿波罗盆地区域具有不同的光谱吸收特征。在阿波罗盆地外,靠近SPA盆缘具有更多Mg辉石吸收特征的短波吸收,而靠近SPA中心区域具有更多高Ca辉石吸收特征的长波吸收。盆地内部不同地质单元的光谱吸收特征也有差异,月海为高Ca辉石的吸收特征,峰环为Mg辉石的短波长吸收。阿波罗盆地具有最薄的月壳厚度、高程差达8 km的地层剖面、位于月球背面SPA盆地内的月海、发育充分的中央峰环,其独特性使它成为最有价值的采样点。
关键词:  阿波罗盆地;南极-艾肯盆地;月壳;光谱
DOI:10.15982/j.issn.2095-7777.2018.05.013
分类号:P691
基金项目:中国科学院B类先导科技专项培育项目(XDB18000000);国家自然科学基金面上项目(41373068,41773065);国家自然科学基金重大项目(41490634);科技部科技基础性工作专项(2015FY210500);Brown University,Office of Vice President for Research SEED grant "Engaging the Chinese Lunar Exploration Program"(CLEP)
Crustal Structure and Spectral Features of Lunar Apollo Basin Region
GUO Dijun1,2,3, LIU Jianzhong1, HEAD W. James3, LI Shuai4, POTTER W. K. Ross3, LIN Honglei2,5
1.Center for Lunar and Planetary Science, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550002, China;2.University of Chinese Academy of Sciences, Beijing 100014, China;3.Department of Earth, Environmental and Planetary Sciences, Brown University, Providence 02912, USA;4.University of Hawaii at Manoa, Honolulu HI 96822, USA;5.Institute of Remote Sensing and Digital Earth, Chinese Academy of Sciences, Beijing 100101, China
Abstract:
The pre-Necterian lunar Apollo impact basin,located inside ancient South Pole-Aitken(SPA)basin,strides the SPA transient cavity and rim. SPA basin is the confirmed largest and oldest basin of the Moon,so the Apollo basin has irreplaceable role in understanding the lunar interior structure and compositions,the local geological processes and the evolutional history of the Moon. The crustal structure of Apollo region is dramatically asymmetric. It's thickening close to SPA rim and thinning close to SPA center,while the thinnest region is inside peak ring of Apollo basin. The absorption features on spectrum are different at different geologic units either. Exterior Apollo basin,the absorption center at locations close to SPA rim tends to be shorter as the Mg pyroxene,while the absorption center at locations close to SPA center tends to be longer as Ca pyroxene. Inside Apollo basin,the spectral features are varying with different spatial locations and geologic units. The maria show absorption feature of Ca pyroxene while the peak ring appears Mg pyroxene rich. The unique characteristics of Apollo basin such as the thinnest crust,the stratigraphic profile as large as 8 km elevation difference,maria erupted from lunar farside,the well-developed peak ring,make it the most valuable sample-return site.
Key words:  Apollo basin;South Pole-Aitken basin;lunar crust;spectrum