| 嫦娥三号着陆区月海玄武岩的年龄、成因及地质意义 |
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| 引用本文： | 李勃,凌宗成,张江,陈剑,孙灵芝,赵昊炜.嫦娥三号着陆区月海玄武岩的年龄、成因及地质意义[J].岩石学报,2016,32(1):19-28. |
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| 作者姓名： | 李勃 凌宗成 张江 陈剑 孙灵芝 赵昊炜 |
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| 作者单位： | 山东大学空间科学研究院, 山东省光学天文与日地空间环境重点实验室, 威海 264209,山东大学空间科学研究院, 山东省光学天文与日地空间环境重点实验室, 威海 264209,山东大学空间科学研究院, 山东省光学天文与日地空间环境重点实验室, 威海 264209,山东大学空间科学研究院, 山东省光学天文与日地空间环境重点实验室, 威海 264209,山东大学空间科学研究院, 山东省光学天文与日地空间环境重点实验室, 威海 264209,大庆油田有限责任公司井下作业分公司, 大庆 163000 |
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| 基金项目： | 本文受国家自然科学基金项目(41373068、U1231103)、科技基础性工作专项(2015FY210500)、山东省自然科学基金项目(ZR2015DQ001、JQ201511)、山东大学基本科研业务费项目(2015ZQXM014、2013ZRQP004)和山东大学(威海)青年学者未来计划(2015WHWLJH14)联合资助. |
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| 摘 要： | 月海玄武岩主要分布在月海中,由斜长石、辉石和橄榄石组成,与地球玄武岩相比,富铁而贫钠和钾。月海玄武岩的成因,年代和成分研究是理解月岩形成与演化的基础。月球返回的岩石样品数量和覆盖面积有限,并且CE-3号着陆区没有月球样品返回,所以地球上的实验室样品分析方法不能应用到CE-3号着陆区玄武岩研究。本文对CE-3号着陆区月表和下伏玄武岩的组分、来源、分布、年代和层序进行反演和分析。主要使用的研究方法主要包括:玄武岩单元的撞击坑频率-分布函数定年,基于撞击坑的月壤下伏玄武岩单元识别、划分及厚度反演,基于遥感数据的元素含量和矿物成分分析等。结果表明:(1)CE-3号着陆区至少出现了6次较大规模的岩浆充填事件,由新到老分别为EIm、EIm_1、EIm_2、Im、Im_1和Im_2,其中EIm单元年龄约为3.17Ga,Im单元年龄为3.48Ga;(2)研究区玄武岩单元铁元素成分变化不大,而钛元素含量有较大变化。并且玄武岩越年轻,铁和钛元素更加富集。对指示月表硅酸盐矿物的克里斯蒂安参数(CF)和弯曲指数(CI)进行计算,发现研究区没有高硅物质的分布;(3)研究区月海玄武岩充填活动具有多期次性,每期月海玄武岩的充填流动大体上保持由南向北方向,并且活动规模逐步减小;(4)下伏玄武岩单元EIm_1、EIm_2、Im、Im_1和Im_2的平均厚度分别为68.3m,68.6m,81.8m,59.1m和52.1m,其中EIm_1单元的厚度最大为150m,从西到东逐渐减小;Im_1最大深度为224m,位于研究区的北部,向东西两侧依次减小。
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| 关 键 词： | 月海玄武岩 成分 厚度和年代 嫦娥三号着陆区 |
| 收稿时间： | 6/9/2015 12:00:00 AM |
| 修稿时间： | 2015/10/12 0:00:00 |
Geochronology, petrogenesis and geological significance of the lunar basalts around CE-3 landing site |
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| LI Bo,LING ZongCheng,ZHANG Jiang,CHEN Jian,SUN LingZhi and ZHAO HaoWei.Geochronology, petrogenesis and geological significance of the lunar basalts around CE-3 landing site[J].Acta Petrologica Sinica,2016,32(1):19-28. |
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| Authors: | LI Bo LING ZongCheng ZHANG Jiang CHEN Jian SUN LingZhi and ZHAO HaoWei |
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| Institution: | Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, China,Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, China,Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, China,Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, China,Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, China and Downhole Service Company, Daqing Oilfield Co. LTD, Daqing 163000, China |
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| Abstract: | Lunar basalts are mainly located in the Maria, and made up of anorthosite, pyroxene and olivine. Different from basalts in Earth, they are rich in Fe and depleted in Na and K. The origin, ages and compositions of the lunar basalts are the basis of understanding the formation and evolution of lunar rocks. The rock samples returned from the Moon have limited numbers and don't cover the CE-3 landing site, thus, the methods of analyzing the rocks in ground labs cannot be used to study lunar basalts. In this paper, our researches focused on the compositions, origin, distribution, age and sequence of basalts in and under lunar surface around CE-3 landing site. The methods we used in this paper included: crater size-frequency distribution, the underlying basalts identification, the compositions derived from the remote sensing data, and so on. The results showed that: (1) There are at least six basaltic filling processes in study area and we can define six basaltic units from young to old which are EIm, EIm1, EIm2, Im, Im1 and Im2. The age of EIm is 3.17Ga, while Im's age is 3.48Ga. (2) Around CE-3 landing site, titanium content changes a lot, while iron content shows a few changes. There is a link between identified basalts' age and their element abundance, which is the younger the age, the more enrichment in titanium and iron. In addition, there is no evidence for high silica materials according to the CF factor and CI index derived from thermal infrared data. (3) The study area has experienced multiple magmatic events, and every fill process flows from south to north and its magnitude reduces gradually. (4) The average thicknesses of five underlying basalts (EIm1, EIm2, Im, Im1 and Im2) are 68.3m, 68.6m, 81.8m, 59.1m and 52.1m separately, and the most thicknesses of EIm1 and lm1 are 150m and 224m. |
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| Keywords: | Lunar basalts Compositions Thickness and age CE-3 landing site |
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