月球样品的中子活化分析技术研究

月球的起源是月球研究的核心问题。月球探测任务返回的数据和样品极大地提高了人类对地月系统的认知,同时也发现了更多未解之谜,亟待未来的探测任务和科学研究来解答。嫦娥五号月壤是我国首次地外天体采集返回的样品,也是继美国和苏联探月采样任务45年后人类再次获得的月球样品。鉴于月球样品的珍贵性和特殊性,利用先进技术开展其全元素含量的非破坏精准分析对于认识月球演化和月球资源就地开发利用具有重要的意义。依托大型核反应研究堆和加速器中子注量率优势,利用中子活化分析技术可实现月球样品中的全元素非破坏分析:1)仪器中子活化分析技术(INAA)可测量Na—U元素之间的60余种元素;2)瞬发γ中子活化分析技术(PGNAA)可补充测量INAA不适合测量的元素如H、B、C、N等;3)中子深度剖面分析技术(NDP)可测量样品近表面(微米级)聚变能源3He的浓度深度分布;4)缓发中子测量技术(DNC)可定量样品中痕量裂变核素如^(235)U和^(239)Pu,并结合INAA可测量238U/235U同位素比值;5)14 MeV快中子活化分析技术(FNAA)可测量INAA和PGNAA不灵敏或不适合测量的元素如O、Si、P等。因此,中子活化分析技术(NAA)可有效解决月球样品中全元素、非破坏和精准测量问题,为我国深空探测珍贵样品研究提供核分析技术支撑。

钙长辉长无球粒陨石GRV 13001中SiO_(2)相的特征及其成因

钙长辉长无球粒陨石中SiO_(2)相的形成与母体经历的热改造作用密切相关,能在一定程度上指示母体的热变质历史。以中国第30次南极科学考察队发现的一块钙长辉长无球粒陨石GRV 13001为研究对象,重点分析了不同产状的SiO_(2)相,发现其可分为成分较纯的不规则粒状方石英和石英、富Al和K的板条状鳞石英以及高钙辉石边部的蠕虫状SiO_(2)相3种类型。不同产状SiO_(2)相的成因及其指示的陨石母体热变质历史为:(1)母星体浅表层岩浆快速冷却结晶,形成充填型不规则粒状方石英;(2)经历缓慢热变质作用形成4型热变质程度辉石,同时导致充填物中部分方石英转变为石英;(3)缓慢热变质作用期间,相对短暂且高温的重新加热事件引起充填物区域物质部分熔融,从而形成板条状鳞石英,亦导致原生辉石颗粒边缘高钙辉石次生边的形成,生长过程中蠕虫状SiO_(2)相被包裹进次生边。不同产状SiO_(2)相的成因为其陨石母体经历的热改造过程提供了依据。

中国南极陨石的收集、研究与展望

陨石不仅是地球与宇宙之间联系的纽带,也是揭开太阳系历史、探索宇宙演化的关键钥匙。南极独特的地理条件和冰雪环境使其成为全球发现陨石最多的地区。自1998年在格罗夫山发现第一个陨石富集区以来,中国已收集了12665块陨石,在全球南极陨石收集数量中排名第三。本文概述了南极陨石发现历史,揭示了冰盖上陨石富集的独特性,集成了中国在格罗夫山陨石收集方面的成绩,并探讨了陨石的分类工作和最新的研究进展。总结取得成就的同时,也探索收集效率下降、富集区域限制和南极陨石自然“消失”等挑战和问题。最后,面对行星科学的快速发展和中国南极秦岭站建成的大好时机,本文提出了一些未来设想,包括成立南极陨石考察队,以秦岭站和中山站为后勤保障基地,开展横贯南极山脉和查尔斯王子山陨石综合考察,并加强南极陨石科研和科普的协同发展。

火星陨石NWA 13763矿物岩石学特征及其岩浆演化

NWA 13763陨石为一块新发现的辉长质辉玻无球粒火星陨石,辉长结构和次辉绿结构,主要矿物组成为辉石(45.1%,其中普通辉石36.1%,易变辉石9.0%)和斜长石(42.3%,几乎全部熔长石化),次要矿物组成为富硅相(5.1%)、橄榄石(2.7%)、磷酸盐矿物(2.4%)、钛铁矿(2.2%),含极少量钛磁铁矿和斜锆石。陨石中广泛发育“铁橄榄石+富硅相”二相后成合晶和“钙铁辉石+铁橄榄石+富硅相”三相后成合晶。辉石主晶核部贫铁富镁(Fs_(24.7-55.3)),边部富铁贫镁(Fs_(61.5-86.1));熔长石成分均一(An_(44.4-54.6Ab43.7-53.7));铁橄榄石(Fa_(84.5-97.7))全部以细粒状分布于后成合晶中。由钛铁氧化物固溶体计算得到岩浆结晶的氧逸度(FMQ)f_(O_(2))=-0.045,钛铁矿结晶温度约975℃。利用全岩成分和MELTS程序模拟计算表明,NWA 13763陨石的母岩浆液相线温度范围可能为1190~830℃,矿物结晶顺序由早到晚可能为:培长石→拉长石→橄榄石→单斜辉石→中长石→磷酸盐矿物→钛铁矿→富硅残余相。

NWA 13943(CK5型)碳质球粒陨石的矿物岩石学和稳定同位素组成研究

CK型陨石是一类高度氧化的碳质球粒陨石,金属/磁铁矿的比值接近零.与其它类型的碳质球粒陨石(岩石类型:1-3)不同,大多数CK型陨石在母体上经历了强烈的热变质过程(550-1270K),以4-6型为主.多项证据表明,CK和CV3型陨石具有成因联系.但是,两者在岩相结构和化学组成方面仍存在微小差异.因此,精细地区分和比较两者的地球化学特征对于验证CK-CV单一母体假说非常重要.Northwest Africa(NWA)13943是一块新发现的陨石,经历过较强烈的热变质作用.利用扫描电子显微镜和电子探针,确定了NWA 13943的岩石类型.并运用质谱分析技术,重点测定了NWA 13943陨石的全岩氧同位素和铬同位素组成.综合岩石结构、矿物化学成分、氧同位素异常(△^(17)O,△代表同位素分馏值)和铬同位素异常(ε^(54)Cr,ε表示样品中的同位素比值与标样中的同位素比值的相对偏差的10^(4)倍),CK和CV型陨石的母体可能形成于原行星盘中两个相似但不同的化学源区.

The Origins of the Arc-Shaped Langshan Uplift and Linhe Trench

In the northern part of the Ordos Basin, there is a 325 km long arc-shaped Langshan uplift and a 15 km-deep Linhe Trench in front of Langshan, which are rare geological phenomena for which origins no one has explained. This article comprehensively analyzes the research achievements over the past 40 years of geology, geomorphology, seismic exploration, paleogeography, and oil and gas exploration in the Ordos Basin and Langshan. It recognizes that the northern part of the Ordos Basin experienced a meteorite impact in the Late Cretaceous period. The impact pushed the block northwest ward, subducting after colliding with igneous rocks in the north. This sudden event formed a clear arc-shaped mountain zone in the north and a wedge-shaped trench in front of the mountain. The chaotic layers, prolonged and continuous faults, and numerous thrust layers in the Langshan, a negative anomaly area in the center of the northern Ordos, abnormal orientation of crystalline basement structures in the north of Ordos, Moho uplift, and distribution of meteorite fragments in the northwest of Langshan, all of these geological phenomena support the occurrence of the meteorite impact event, forming the arc-shaped Langshan and the Trench.

Machine learning applications on lunar meteorite minerals:From classification to mechanical properties prediction

Amid the scarcity of lunar meteorites and the imperative to preserve their scientific value,nondestructive testing methods are essential.This translates into the application of microscale rock mechanics experiments and scanning electron microscopy for surface composition analysis.This study explores the application of Machine Learning algorithms in predicting the mineralogical and mechanical properties of DHOFAR 1084,JAH 838,and NWA 11444 lunar meteorites based solely on their atomic percentage compositions.Leveraging a prior-data fitted network model,we achieved near-perfect classification scores for meteorites,mineral groups,and individual minerals.The regressor models,notably the KNeighbor model,provided an outstanding estimate of the mechanical properties—previously measured by nanoindentation tests—such as hardness,reduced Young’s modulus,and elastic recovery.Further considerations on the nature and physical properties of the minerals forming these meteorites,including porosity,crystal orientation,or shock degree,are essential for refining predictions.Our findings underscore the potential of Machine Learning in enhancing mineral identification and mechanical property estimation in lunar exploration,which pave the way for new advancements and quick assessments in extraterrestrial mineral mining,processing,and research.

Micromechanical testing and property upscaling of planetary rocks:A critical review

Knowledge of the mechanical behavior of planetary rocks is indispensable for space explorations.The scarcity of pristine samples and the irregular shapes of planetary meteorites make it difficult to obtain representative samples for conventional macroscale rock mechanics experiments(macro-RMEs).This critical review discusses recent advances in microscale RMEs(micro-RMEs)techniques and the upscaling methods for extracting mechanical parameters.Methods of mineralogical and microstructural analyses,along with non-destructive mechanical techniques,have provided new opportunities for studying planetary rocks with unprecedented precision and capabilities.First,we summarize several mainstream methods for obtaining the mineralogy and microstructure of planetary rocks.Then,nondestructive micromechanical testing methods,nanoindentation and atomic force microscopy(AFM),are detailed reviewed,illustrating the principles,advantages,influencing factors,and available testing results from literature.Subsequently,several feasible upscaling methods that bridge the micro-measurements of meteorite pieces to the strength of the intact body are introduced.Finally,the potential applications of planetary rock mechanics research to guiding the design and execution of space missions are environed,ranging from sample return missions and planetary defense to extraterrestrial construction.These discussions are expected to broaden the understanding of the microscale mechanical properties of planetary rocks and their significant role in deep space exploration.

Meteorite classification for building the Chinese Antarctic Meteorite Depository Introduction of the classification of 500 Grove Mountains meteorites

Meteorites provide an important window into the origins and evolution of the solar system. Since the first four meteorites were recovered in Grove Mountains, Antarctica, in 1998, a further total of 12665 meteorites have been collected over seven polar seasons in the Grove Mountains. All of these meteorites are owned and managed by the Chinese Antarctic Meteorite Depository （CAMD） at the Polar Research Institute of China （PRIC）. In recent years, another 500 Antarctic meteorites have been classified and characterized based on mineralogy and petrology. In this work we examine four samples that have been identified as terrestrial, and a further 496 samples that have been confirmed as meteorites. These meteorites are further divided into different types：488 ordinary chondrites, one eucrite, one ureilite, one CM2 carbonaceous chondrite, one EH4 enstatite chondrite, one mesosiderite and three iron meteorites. The classification of meteorites not only provides an abundance of fundamental scientific data, but is also significant for introducing meteorites and related scientific knowledge to the publics particularly via the website of Chinese Resource-sharing Platform of Polar Samples for scientific research and education.

Progress in study of Chinese Antarctic Meteorites

This paper reviews and summarizes the Chinese Antarctica meteorite search, classification and research. During the past four antarctic explorations, a total of 9834 meteorites were collected in the Grove Mountains region. Among them, 2431 meteorites were classified by the end of 2008. So far, 684 meteorites have been officially published in the Meteoritical Bulletin, Meteoritical Society, including 2 martian meteorites, 2 eucrites, 6 ureilites, 5 mesosiderites, 1 pallasite, 1 iron and 10 carbonaceous chondrites. Comprehensive studies were carried out on a number of these rare type meteorites. In addition, we propose to continue the meteorite searching project in Grove Mountains and other regions in Antarctica. We also suggest several key topics of the future researches on the Chinese Antarctic meteorites.

Lunar meteorites: witnesses of the composition and evolution of the Moon

Lunar meteorites are fragments of the Moon that escaped the gravity of the Moon following high-energy impacts by asteroids, subsequently fell to Earth. An inventory of 165 lunar meteorites has been developed since the discovery and identification of the first lunar meteorite, ALHA 81005, in 1979. Although the Apollo samples are much heavier in mass than lunar meteorites, the meteorites are still an important sample supplement for scientific research on the composition and history of the Moon. Apart from a small amount of unbrecciated crystalline rocks, the majority of lunar meteorites are breccias that can be classified into three groups： highland feldspathic breccia, mare basaltic breccia, and mingled（including fledspathic and basaltic clasts） breccia. The petrography of lunar rocks suggests that there are a series of rock types of anorthosite, basalt, gabbro, troctolite, norite and KREEP in the Moon. Although KREEP is rare in lunar rocks, KREEP components have been found in the increasing number of lunar meteorites. KREEP provides important information on lunar magmatic evolution, e.g., the VHK KREEP clasts in SaU 169 may represent the pristine lunar magma （urKREEP）. Six launching pairs of lunar meteorites have been proposed now, along with ten possible lunar launching sites. In addition, symplectite is often found in lunar basalts, which is a significant record of shock metamorphism on the lunar surface. Furthermore, isotopic ages and noble gases not only provide information on crystallization processes in lunar rocks and the formation of lunar crust, but also provide insight into shock events on the lunar surface.

Classification of Grove Mountains meteorites and its significance

Meteorites are the extraterrestrial rocks, which provide insights into the origin and evolution of the solar system. During the past half century, a great number of meteorites has been discovered on the Antarctic Ice Sheet, confirming that the Antarctica is the most important meteorite concentration area on the earth. Since the first four Antarctic meteorites were found in Grove Mountains in 1998, a total of 9834 meteorites have been collected by four subsequent expeditions. It opens a new field of meteorite study in China, and also accumulates a great deal of scientific samples for China. Recently, classification of Grove Mountains meteorites has been carried out for 6 years, and made following progresses ： （ 1 ） 2433 meteorites, which include many special meteorites, e.g. Martian meteorites, ureilites and carbonaceous chondrites, have been classified. （2） the Antarctic meteorite curation and the sample sharing system are set up preliminarily. （3） the classification procedure, the management of meteorite samples, and the application procedure for the Antarctic meteorites are completed after the systematic classification during these years. （4） young generation researchers on meteorite are trained through the cooperation of many universities and institutes on meteorite classification.

Chemical compositions and cassfication of Grove Mountains(GRV)98003 and other Chinese iron meteorites

Concentrations of Cr, Co, Ni, Cu, Ga, Ge, As, Sb, W, Re, Ir, Pt and Au of two ungrouped iron meteorites, Grove Mountains （GRV） 98003 from Antarctica and Ujimqin, were measured using instrumental neutron activation analysis. According to the bulk chemistry, GRV 98003 is classified as a member of ⅠAB group, and Ujimqin as a unique one of ⅠAB iron meteorite complex. The elemental abundance pattern and correlation between elements （e. g. Ni-Au, Co-Au, As-Au, W- Au, Cu-Au, Sb-Au） of GRV 98003 are similar with those of NAW 468 （ⅠAB）, but significantly depleted in refractory siderophile elements （ Re, It） and moderate volatile elements （Ca, Ge） relative to the latter. In addition, we reclassify Nantan （ⅢCD） as a member of ⅠAB main group （MG） and Yongning （ⅠA） as a unique iron meteorite related with IAB iron meteorite complex.

Siderophile Element Compositions of Pyroxenes in HED Meteorites: Implications for the Differentiation of Magma Ocean on Vesta

1 Introduction The howardite,eucrite and diogenite(HED)meteorites are ultramafic and mafic igneous rocks and impact-engendered breccias derived from a thoroughly differentiated asteroid 4 Vesta.Diogenites include dunites,

Challenges of identifying putative planetary-origin meteorites of non-igneous material

This paper summarizes the challenges of identifying planetary-origin meteorites of non-igneous composition - particularly those of sedimentary origin.Evidence for putative sedimentary-origin (sedtype) meteorites and their potential parent bodies is reviewed,suggesting that the list of candidate parent bodies for sed-type meteorites includes,but is not limited to,Mars,Enceladus,Ganymede,Europa,Ceres,Vesta,and other hypothetical planets that existed between the orbits of Mars and Jupiter in the past.The extraterrestrial origin and probable parent body for sed-type meteorites should be assessed based on multiple lines of evidence,and not solely limited to tests of oxygen and noble gas isotopes,whose signatures may undergo terrestrial contamination and which may exhibit significant heterogeneity within both the Solar System and parent cosmic bodies.The observed fall of a cosmic body,evidence of hypervelocity fall,signs of impact,presence of fusion crust,melting,and/or shock deformation features in impactor fragments should be considered as priority signs of meteoritic origin.

MOSSBAUER SPECTROSCOPIC STUDY OF FIRED SHENQIU METEORITES

The Shenqiu meteorite was investigated by Mossbauer spectroscopy at room temperature, atomic absorption, X-ray diffraction and scanning electron microscopy. In order to determine fired conditions of the meteorite which occurred during the meteorite fall, Shenqiu meteorite samples were fired in an oxidizing atmosphere and a reducing atmosphere at temperatures up to 1300℃, respectively. These samples also were fired at 800, 1000 and 1200 ℃ respectively for different time (up to 24 h).

Meteorites from Grove Mountains, Antarctica:An overview

Thirty-two meteorites were collected in Grove Mountains area, Antarctica, by the 15th and 16th Chinese Antarctic Research Expeditions (CHINARE). Petrography and mineral chemistry of these meteorites are reviewed, among which there are one Martian lherzolite, one eucrite, one ungrouped iron meteorite, and six unequili-brated and twenty-three equilibrated ordinary chondrites. An equilibrated ordinary chondrite GRV 98004 ( H5 ) has an unusually low cosmic-ray exposure age. Meteorite concentrating processes in Grove Mountains area are discussed. In addition, future studies on Grove Mountains (GRV) meteorites are proposed.

The chemical compositions of Antarctic iron meteorites and their classification

The concentrations of 13 elements in the metal of 52 Antarctic irons have been reported and these irons have been classified based on the structures and their Ga,Ge, Ni, Ir and other trace elemental contents. The 52 iron meteorites assigned to chemical group consist of 16 of ⅠAB,12 of ⅡAB, 1 of ⅡE,3 of ⅢAB, 1 of ⅢCD, 1Of ⅣA and 18 of ungrouped irons. The ⅠAB, ⅢCD and ⅡE iron meteorite groups areconsidered to be of nonmagmatic origin. Nonmagmatic ⅠAB, ⅢCD and ⅡE ironsformed as individual pools of a chondritic body. The other groups, ⅡAB, ⅢAB andⅣA show the evidences of having originated by fractional crystallization of a metallicmagma.The slopes on element-Ni trends in the magmatic are generally higher than inthe nonmagmatic groups. Most interestings are the high abundance Of ungrouped andⅠAB (47.2% and 27.8%,respectively) and low abundance of ⅢAB (5.8%).Antarctic irons of the group abundances can be distinguished from non-Antarctic irons,which provide the information about previously unsampled parent planets, mass,shockand collision,as well as nebula regions.

Shock metamorphism in meteorites

Shock metamorphism resulting from hyperveloeity collisions between planetary bodies, is a fundamental processes in the solar system. The term ＂shock metamorphism＂ is used to describe all changes in rocks and minerals resulting from the passage of shock waves. Most meteorites have experienced coUisions and have a record of shock metamorphism, which includes brecciation, deformation, phase transformation, local melting and crystallization. The key to reading this record is to use the shock features to estimate the pressure and duration of shock event. In this paper, the history of the study of shock metamorphism is reviewed; basic knowledge of shock physics is discussed; recent 10 years＇ studies of shock-induced melt veins are summarized; and finally a short note to the shock metamorphism in general is given.

Alpha Centauri System and Meteorites Origin

We propose a mathematical model for determining the probability of meteorite origin, impacting the earth. Our method is based on axioms similar to both the complex networks and emergent gravity. As a consequence, we are able to derive a link between complex networks and Newton’s gravity law, and as a possible application of our model we discuss several aspects of the Bacubirito meteorite. In particular, we analyze the possibility that the origin of this meteorite may be alpha Centauri system. Moreover, we find that in order for the Bacubirito meteorite to come from alpha Cen and be injected into our Solar System, its velocity must be reduced one order of magnitude of its ejected scape velocity from alpha Cen. There are several ways how this could happened, for example through collision with the Oort cloud objects (located outside the boundary of our Solar System), and/or through collisions within the Solar meteorites belt (located between Mars and Jupiter). We also argue that it may be interesting to study the Bacubirito meteorite from the perspective of the recently discovered Oumuamua object.