Ages of lunar impact breccias: Limits for timing of the Imbrium impact

Since the Apollo 14 mission delivered samples of the Fra Mauro formation, interpreted as ejecta of the Imbrium impact, defining the age of this impact has emerged as one of the critical tasks required for the complete understanding of the asteroid bombardment history of the Moon and, by extension, the inner Solar System. Significant effort dedicated to this task has resulted in a substantial set of ages centered around 3.9 Ga and obtained for the samples from most Apollo landing sites using a variety of chronological methods. However, the available age data are scattered over a range of a few tens of millions of years, which hinders the ability to distinguish between the samples that are truly representative of the Imbrium impact and those formed/reset by other, broadly contemporaneous impact events. This study presents a new set of U-Pb ages obtained for the VHK (very high K) basalt clasts found in the Apollo 14 breccia sample 14305 and phosphates from (i) several fragments of impact-melt breccia extracted from Apollo 14 soil sample 14161, and (ii) two Apollo 15 breccias 15455 and 15445. The new data obtained for the Apollo 14 samples increase the number of independently dated samples from this landing site to ten. These Apollo 14 samples represent the Fra Mauro formation, which is traditionally viewed as Imbrium ejecta, and therefore should record the age of the Imbrium impact. Using the variance of ten ages, we propose an age of 3922 ± 12 Ma for this event. Samples that yield ages within these limits can be considered as possible products of the Imbrium impact, while those that fall significantly outside this range should be treated as representing different impact events. Comparison of this age for Imbrium (determined from Apollo 14 samples) with the ages of another eleven impact-melt breccia samples collected at four other landing sites and a related lunar meteorite suggests that they can be viewed as part of Imbrium ejecta. Comprehensive review of ⁴⁰Ar/³⁹Ar ages available for impact melt samples from different landing sites and obtained using the step-heating technique, suggests that the majority of the samples that gave robust plateau ages are indistinguishable within uncertainties and altogether yield a weighted average age of 3916 ± 7 Ma (95 % conf., MSWD = 1.1; P = 0.13) and a median average age of 3919 + 14/-12 Ma, both of which agree with the confidence interval obtained using the U-Pb system. These samples, dated by ⁴⁰Ar/³⁹Ar method, can be also viewed as representing the Imbrium impact. In total 36 out of 41 breccia samples from five landing sites can be interpreted to represent formation of the Imbrium basin, supporting the conclusion that Imbrium material was distributed widely across the near side of the Moon. Establishing temporal limits for the Imbrium impact allows discrimination of ten samples with Rb-Sr and ⁴⁰Ar/³⁹Ar ages about 50 Ma younger than 3922 ± 12 Ma. This group may represent a separate single impact on the Moon and needs to be investigated further to improve our understanding of lunar impact history.     

月球撞击坑自动识别和分类方法研究进展

撞击坑是研究月球最直接的对象,也是月球表面最为普遍且显著的地貌单元和地质构造标志,在行星地质学研究中具有重要的地位。通过对月球撞击坑识别方法和撞击坑分类方法研究进展进行概述及总结,将月球撞击坑识别方法概括为人工识别、基于形态特征提取算法、基于机器学习算法、基于地理信息融合分析算法4类,并对月球撞击坑识别方法研究中存在的问题进行了分析。     

Apollo 11月壤样品中太阳风成因的水及其意义

为研究太阳风成因水在月表低纬度地区的分布特征,本文对中国科学院地质与地球物理研究所博物馆珍藏的一份Apollo 11月壤样品开展了单颗粒原位纳米离子探针H同位素和水含量深度剖面分析。结果表明月壤颗粒表层（< 200nm）具有较高的水含量（剖面最大水含量变化范围为0.35%~1.59%,平均值为0.82%）,该结果与前人对Apollo样品的报导类似。除一颗斜长石的H同位素组成（δD=-262‰）落在月幔范围内,其余颗粒表层均非常贫D（δD变化范围为-987‰~-642‰）。该强烈贫D的同位素组成与太阳风一致,完全不同于地球大气水,不仅证明这些样品的月球来源,并且主要是太阳风注入的贡献。矿物颗粒之间的水含量和δD值变化,很可能与太阳风注入后的扩散丢失程度不同有关。另外,我们观察到橄榄石、单斜辉石和长石的水含量剖面比较类似,整体呈现随深度逐渐递减的趋势。相比之下,玻璃质颗粒的水含量剖面呈现随深度先上升再降低的峰形特征,峰位在25~43nm深度。这两者之间的差异很可能跟H在矿物和玻璃中的扩散速率、辐射损伤层等的差异有关。本项研究也证明,即使对于H这样易于受地球污染的元素,在普通条件下（北京、瓶中密封）经过长达50多年的时间,仍能很好地保存注入月壤颗粒中的太阳风信息。但是低温、干燥和真空/惰性气体环境仍是长期保存的有利条件。

     

Noble Gases in the Lunar Regolith

The most fundamental character of lunar soil is its high concentrations of solar-wind-implanted elements, and the concentrations and behavior of the noble gases He, Ne, Ar, and Xe, which provide unique and extensive information about a broad range of fundamental problems. In this paper, the authors studied the forming mechanism of lunar regolith, and proposed that most of the noble gases in lunar regolith come from the solar wind. Meteoroid bombardment controls the maturity of lunar soil, with the degree of maturation decreasing with grain size; the concentrations of the noble gases would be of slight variation with the depth of lunar soil but tend to decrease with grain size. In addition, the concentrations of noble gases in lunar soil also show a close relationship with its mineral and chemical compositions. The utilization prospects of the noble gas ^3He in lunar regolith will be further discussed.     

月壤中纳米金属铁的太空风化成因及模拟方法分析

月壤中普遍存在着大量由太空风化作用产生的纳米金属铁,这些纳米金属铁在一定程度上改变了月球表面的物理、化学和光学特征.纳米金属铁在月壤中主要赋存于胶结质玻璃相中和月壤颗粒的表面,胶结质玻璃相的纳米金属铁起源于微陨石轰击富含太阳风氢粒子的月壤产生的高温熔融还原作用,颗粒表面的纳米金属铁来自微陨石轰击引起的蒸发沉积作用和太阳...     

月壤中的稀有气体

月球极度亏损挥发分,但是月壤中赋存有大量的稀有气体,主要来源于太阳风注入、宇宙射线作用和放射性同位素衰变等过程。月岩和月壤样品的稀有气体研究,不仅是获取月球表面形成和演化历史、近地空间小行星撞击历史等的重要内容,更是解译40亿年以来太阳风演化的惟一可行途径。本文主要介绍月岩和月壤中的太阳风记录、宇宙射线暴露年龄、Ar-Ar定年以及稀有气体测试技术等方面研究的进展。     

月球雨海地区玄武质岩浆充填活动期次的重新厘定及地质意义

雨海盆地是月球上研究程度最高的多环结构盆地,月球上古老的和年轻的玄武岩在盆地中均有分布,因此雨海是研究月海玄武岩岩浆活动的理想区域。为了更合理的厘定雨海地区的玄武质岩浆演化历史,本文主要结合岩石学、年代学等工作对本区玄武岩的充填期次进行重新划分。利用嫦娥一号IIM光谱数据进行岩石类型分布图编制,初步划分了5类不同钛含量的月海玄武岩;基于高分辨率100m LRO宽视角影像数据通过撞击坑尺寸-频率定年法(CSFD)对本区玄武岩单元模式年龄进行厘定,共划分35个玄武岩单元,发现本区在3.49~2.23Ga均有玄武质岩浆充填活动,具有多期次性。在建立不同类别玄武岩、形貌特征与模式年龄的对应关系基础上,将玄武岩充填划分为4个期次:极低钛玄武岩(3.49~3.20Ga)、低钛玄武岩(3.29~2.83Ga)、中钛玄武岩(3.13~2.52Ga)、(极)高钛玄武岩(2.92~2.23Ga)。本区地形地貌高程特征与不同表面年龄的玄武岩单元之间总体上呈现出一定的负相关性。因此在本区玄武质岩浆期次划分考虑上,不仅要考虑玄武岩的成分特征,更要考虑结合与玄武岩演化密切相关的年代学及形貌学特征,利用形貌、成分数据和年代学信息来共同约束玄武质岩浆期次划分及演化历史。     

月球东海盆地的矿物光谱特征及遥感探测

东海盆地是月球上最年轻的大型撞击盆地之一,其地形地貌和矿物与岩石类型分布将有助于我们深入理解月球撞击盆地形成过程和地质演化历史。LOLA高程数据揭示东海盆地为保存完好的多环撞击盆地。基于月球矿物绘图仪（M3）反射率数据,在东海盆地发现了尖晶石、辉石、结晶斜长石、橄榄石等矿物,采用修正高斯模型（MGM）进行混合矿物光谱分解获取了矿物端员,利用光谱角分类方法（SAM）作出了Maunder 撞击坑的主要矿物分布图。发现的纯结晶斜长石矿物与最近其他月球探测（如Kaguya)相吻合,为月球岩浆洋模型提供了新约束条件。在Lowell撞击坑中央峰发现尖晶石分布,并利用多光谱成像仪（MI）数据进行了验证;利用MGM方法,在Maunder建造上发现结晶斜长石与尖晶石的混合矿物,我们通过分析认为东海盆地的尖晶石在外卢克山脉上可能有更广泛的分布。     

微波雷达在嫦娥探月工程中的应用

微波穿透雷达对月球的观测方式可以分为地基、星载环绕、星地联合以及就位探测等。对比其他探测手段,微波雷达在探测范围和空间分辨率上有很明显的优势,因此在月球和其他行星探测中起着重要的作用。国内外越来越多的深空探测任务已经或准备携带微波雷达,用于探索地外天体的浅表层地质结构,以了解行星地质过程和演化历史。本文综述了我国嫦娥三号和四号月球车玉兔号和玉兔2号在就位微波雷达(测月雷达)探测月球浅表层地质结构方面所取得的新进展,重点阐述了测月雷达在揭示月壤内部的精细结构、表层与次表层地质结构探测等方面的应用。最后,展望了我国月球微波雷达的发展趋势。     

干旱戈壁区金属元素的垂向变化与分散——以新疆金窝子金矿为例

本文选择被风化物覆盖(4米至几十米厚)的金窝子金矿作为研究对象。分析矿体上方风化层和非矿上方的垂直剖面中的各种金属元素的总量及活动态含量,以获得金属元素在风化层中的活动规律,为化探找矿提供方法依据。结果发现金等的某种活动态的分布模式在矿体上方呈现双层分布,即他们趋向于在垂直剖面的底部与顶部富集,而在中部降低。可以解释为元素在剖面底部风化层中的富集是由于金继承了矿体的风化产物,而在地表或近地表的富集是由于从矿体迁移至地表的元素被粘土物质和铁锰氧化物膜所吸附。     

Not so rare Earth? New developments in understanding the origin of the Earth and Moon

A widely accepted model for the origin of the Earth and Moon has been a somewhat specific giant impact scenario involving an impactor to proto-Earth mass ratio of 3:7, occurring 50-60 Ma after T₀, when the Earth was only half-accreted, with the majority of Earth's water then accreted after the main stage of growth, perhaps from comets. There have been many changes to this specific scenario, due to advances in isotopic and trace element geochemistry, more detailed, improved, and realistic giant impact and terrestrial planet accretion modeling, and consideration of terrestrial water sources other than high D/H comets. The current scenario is that the Earth accreted faster and differentiated quickly, the Moon-forming impact could have been mid- to late in the accretion process, and water may have been present during accretion. These new developments have broadened the range of conditions required to make an Earth-Moon system, and suggests there may be many new fruitful avenues of research. There are also some classic and unresolved problems such as the significance of the identical O isotopic composition of the Earth and Moon, the depletion of volatiles on the lunar mantle relative to Earth's, the relative contribution of the impactor and proto-Earth to the Moon's mass, and the timing of Earth's possible atmospheric loss relative to the giant impact.     

基于辐射传输模型的月表铁镁质矿物定量反演:以嫦娥三号着陆区为例

我国嫦娥三号着陆于雨海北部的年轻玄武岩熔岩平原上,该区域的物质成分和矿物组成对于理解月球年轻的火山活动具有重要研究价值。月球全球勘探者(Lunar Prospector,LP)探测的元素数据揭示着陆区附近岩石类型主要为高铁中钛玄武岩(19.5%FeO;5.2%TiO_2)。本研究利用月球矿物绘图仪(Moon Mineralogy Mapper,M~3)获取的嫦娥三号着陆区附近的新鲜撞击坑高光谱数据,采用Hapke辐射传输模型和修正高斯模型(MGM)联合分析,对其年轻月海玄武岩铁镁质矿物进行了定量反演。研究表明该区域玄武岩中矿物组成以单斜辉石矿物为主,存在较高比例的橄榄石。基于光谱库匹配方法和MGM优化分析,我们反演出单斜辉石,斜方辉石,橄榄石和钛铁矿四种矿物的相对体积比为57.6:18.0:15.3:9.1,这一研究结果有待于与嫦娥三号玉兔号月球车上搭栽的红外成像光谱仪数据进行比对,以期从遥感和就位探测两个角度获得对于该地区矿物和岩石类型的全面认识。     

蒙古国伊罗河铁矿床地质特征及找矿标志

蒙古国伊罗河铁矿床属于华力西晚期形成的接触交代型铁矿床,探获资源量近10×10⁸t,矿床平均品位＞50%,外围有多个探明铁矿产地及找矿远景区,周边潜在资源量30×10⁸~40×10⁸t。为探讨该区域接触交代型铁矿床的成矿地质规律,本文从伊罗河铁矿的成矿地质背景、矿区地层、构造、岩浆岩、变质作用分析入手,以其东矿段Ⅰ号矿体为例详细论述矿体形态、规模、产状、赋矿岩性特征,通过矿石样品测试分析阐述矿物组成特征、化学成分、矿石结构构造、磁铁矿粒度及成矿阶段等,初步总结了矿床成因和找矿标志。     

珠江三角洲潜在生态风险:土壤重金属活化

珠江三角洲典型土壤模拟酸雨提取实验表明，土壤酸缓冲能力为菜园土大于水稻土大于赤红壤。酸化过程早期，铝铁胶体吸附共沉淀导致重金属溶出量增长不明显甚至下降；进一步酸化时，多数元素溶出量与加入酸量呈显著正相关。计算表明，在pH=4．5的酸雨作用下，溶液中Hg、Mn、Pb、Fe(以Fe2O3表示)浓度已超出Ⅱ级地表水标准，Cu、Zn大大高于渔业用水标准。可见，土壤元素活化溶出对水体生态环境有潜在的危害。     

西宁盆地咸水湖相沉积型富硒土壤的形成机理及意义

通过对西宁盆地土壤和岩石Se的调查分析发现,古近系西宁组和白垩系民和组岩石及发育的土壤中Se值最高,是西宁盆地土壤主要的富硒母质。进一步结合西宁盆地退缩过程中的古地理资料,西宁盆地由干旱炎热的咸水湖相到湿润冷凉的咸水—淡水湖相对应沉积了古近系西宁组和新近系贵德群,Se在咸水湖边界和干旱炎热的咸水湖相环境的共同作用下,并经地貌、水系等改造,形成了西宁盆地咸水湖相沉积型富硒土壤的现有格局。该类型富硒土壤有重金属低、Se含量适中、有效Se高等优势,具有较好的开发利用价值。     

高精度磁测在山西孤山隐伏铁矿勘查中的应用

山西孤山铁矿是被长城系高于庄组白云岩和第四系覆盖的全隐伏矿床。通过地面高精度磁法测量,获取了磁异常数据,圈定了磁异常范围,磁异常总体呈NE走向,长约4000m,平均宽约800m。通过化极、不同高度的延拓处理和拟合反演,根据异常特征结合地质资料分析,确定了隐伏磁铁矿的分布和空间特征,为矿床进一步勘探和开发提供了地球物理依据。     

云南郎都铜矿地质特征与矿床成因分析

郎都铜矿位于义敦-中甸岛弧带南段,红山复式背斜北东翼。矿体主要赋存于张性破碎带、层间破碎带、褶皱的转折端以及外接触带。矿床的形成与围岩性质、构造破碎带和围岩蚀变类型有较为直接的联系。矿床类型属接触交代热液型铜矿床,与成矿有密切关系的岩体为石英二长斑岩,围岩为碳酸盐岩类中的灰岩类,典型的矽卡岩矿物为透辉石,其次为石榴子石,其中透辉石矽卡岩含矿性明显高于石榴子石矽卡岩。根据同位素研究成果,郎都铜矿的成矿年龄大致为214.8±3.8 Ma;成矿的大地构造环境属于造山带环境。成矿物质主要来源为下地壳,次为地幔,具备壳幔混合和深源-浅源混合的特征。矿床的形成是多期次交代作用叠加的结果,具典型的矽卡岩型铜矿床基本特征。     

安徽省当涂县九连山铁矿地质特征与找矿标志

多年来在宁芜地区发现了大量的玢岩型铁矿床。九连山铁矿位于和睦山铁矿与钟山铁矿之间,铁矿体主要产于三叠系黄马青组粉砂岩与闪长岩体的接触带,以及黄马青组的层间破碎带;矿区共有10个铁矿体,矿体呈似层状、透镜状,大部分为磁铁矿体,少量的赤铁矿体,矿石多为块状构造和浸染状构造。研究认为,九连山深部成矿的闪长岩体与和睦山的成矿岩体为同一岩体,九连山铁矿可作为和睦山式铁矿埋深较大的矿床实例,矿床类型属于玢岩铁矿中的接触交代型+热液充填型铁矿床。文章还对九连山铁矿的找矿标志进行了归纳。     

郴州市玛瑙山铁锰多金属矿床地质特征

玛瑙山铁锰多金属矿床产于棋梓桥组底部层位中，矿体呈似层状。除铁、锰、铅外，伴生有银、铟。由泥盆纪沉积期成岩成矿作用和燕山期岩浆热液叠加成矿作用所形成的沉积改造—岩浆热液叠加型铁锰多金属矿床。     

青海省东昆仑西段尕林格铁多金属矿床特征及成因

尕林格铁多金属矿床是位于青海省东昆仑西段祁漫塔格断褶带内典型的铁矿床,其成矿作用主要受特定层位地层、同生同质角砾岩和火山岩一次火山岩控制,矿体主要分布在O．St^a-2和O．St^a-4大理岩岩性段中,与矿化关系密切的围岩蚀变主要是矽卡岩化和蛇纹石化。矿石矿物主要为磁铁矿,其次为赤铁矿和菱铁矿。成因类型属于火山喷气沉积一叠加改造型矿床。