热力学计算模拟对初始月幔结构的约束SCIEI北大核心CSCD

月球岩浆洋结晶形成的初始月球内部结构是其后续演化过程的开端,其结晶过程受月球岩浆洋的初始深度和物质组成这两个参数的制约。由于缺少直接来自月球深部的岩石样品,目前关于月球岩浆洋演化过程的探讨主要依赖实验和计算模拟手段。岩浆洋模型中形成的月壳厚度是否与探测结果一致是月球岩浆洋演化模型合理性的重要约束。最新的GRAIL(Gravity Recovery and Interior Laboratory)探测数据推算月壳厚度为34~43km,低于阿波罗时期认为的约70km,这对已有的月球岩浆洋演化模型提出了挑战。本文采用并修正FXMOTR程序包,针对月球岩浆洋在不同的初始深度和物质组成情况下的结晶过程,进行了一系列热力学计算模拟。通过量化月球岩浆洋的初始深度和物质组成对月壳厚度的影响,结合关于月球内部微量元素分配的研究结果,对比了月球岩浆洋结晶后期的残余熔体与原始克里普组分(urKREEP)的成分。本文的模拟结果显示,一个全月幔熔融且初始成分为月球初始上月幔组成(LPUM)的岩浆洋将在其深部结晶2.5%石榴子石,形成的月壳厚度符合GRAIL的约束,并且结晶出了合适的urKREEP成分。在此模型的基础上获取了月球初始的内部成分和密度结构,并对后期月幔翻转(Overturn)的程度进行了探讨。     

存在初始“传导盖层”的月球岩浆洋演化与月壳成因

月球早期经历了岩浆洋阶段,岩浆洋的研究对认识月球内部构造有着重要意义。月球岩浆洋演化主导模型认为:岩浆洋结晶到80%左右,斜长石开始结晶,并上浮形成斜长岩月壳。该模型与观察事实存在两点矛盾:1)基于该模型计算结晶的斜长石An牌号比高地样品斜长石An牌号测试结果低;2)该模型散热速率计算指示岩浆洋在几个百万年时间内固化,而同位素体系对月球岩石样品定年结果表明月壳的结晶年龄十分古老,并且结晶区间跨越了270Myr,这与主导模型之间存在矛盾。以解决以上两点矛盾为目的,本文论证岩浆洋在演化之初硕部存在冷却"盖层",并将硅酸盐熔体在温度梯度下的热扩散效应引入岩浆洋演化模型。热扩散效应指均一的物质在温度梯度下发生分异的过程。本文工作模型是:由于月球的重力常数小,不能有效的保持大气,因此月球的岩浆洋表面温度很低。此时岩浆洋自上而下存在一个过渡的瞬态固化"盖层"(淬火层),岩浆洋自上而下存在温度梯度,岩浆洋在该梯度下发生热扩散效应(Soret效应),Soret效应导致上部结晶斜长石的熔体富Ca和贫Na,因此结晶的斜长石An牌号高。     

岩浆岩中的熔体包裹体

熔体包裹体是岩浆岩矿物生长过程中捕获的天然岩浆珠滴 ,它们有效地保存了大量有关其主矿物形成时周围岩浆介质的物理化学信息 ,所以它们是其主矿物结晶演化史的忠实记录员 ,它们能够提供岩浆系统成分和演化的重要信息。文中对熔体包裹体研究的若干基本原理进行了讨论 ,它们涉及 :(1)熔体包裹体的一般特征 ;(2 )熔体包裹体封闭过程中和封闭后的演化 ;(3)熔体包裹体的均一化研究 ;(4 )熔体包裹体化学成分和挥发组分研究。熔体包裹体研究可以对岩浆岩石学中的一些重要问题进行更为深入的探索 :(1)重建天然岩浆结晶演化的热历史 ;(2 )提供有关岩浆沿下降液相线的成分数据 ;(3)查明天然岩浆结晶演化过程中化学成分的变迁规律 ;(4 )解决岩浆岩石学中的一些疑难问题 ,如岩浆不混溶作用、岩浆混合作用、岩浆混染作用、岩浆中硫的性状、地幔部分熔融和地幔交代作用等方面的问题。将熔体包裹体数据和常规的岩石学、地球化学和实验岩石学信息综合一体 ,可以提高我们模拟岩浆作用过程的能力。熔体包裹体研究已经成为现代岩浆岩石学的一个独立的分支 ,其前景十分广阔。     

热力学计算模拟对月球镁质岩套源区的约束

镁质岩套是月球上最重要的岩石之一.通常认为该类岩石的母岩浆来自月幔翻转引起的深部物质的减压熔融或者月壳底部的混合杂化.但是,这两类模型分别面对无法重现样品中橄榄石的Cr203含量过低等地球化学特征,也无法解释镁质岩套与其他月球样品年龄重合的问题.本文采用热力学计算方法,通过改变源区物质组成、熔融程度、熔融方式及结晶方式等参数,对两种模型进行了一系列的正演研究.结果 表明,月球的镁质岩套有多种成因:月幔物质减压熔融形成的熔体通过平衡结晶可以形成镁质岩套,并满足样品中橄榄石Cr2O3含量的制约;减压熔融模型可以解释某些月球样品年龄的重合,但是成分较为单一,而混合杂化模型形成的镁质岩套成分范围较广.     

月球的构造演化：嫦娥月图解释的理论基础

基于月球研究资料的整理、综合及嫦娥1月图影像的实例解读和解释,本文介绍并总结了月球的构造及演化研究的若干概念、研究思路和新的观点。通过纲要性勾画,描绘月球不同类型和阶段构造演化的基本轮廓,重点论述了四个方面的问题：对月面建造历史和月球演化的历史进行了修正,将月球演化按照其特点三分为冥、古、新月宙／界,并提出建立南海纪／系的主张;以东海Hevelius抛射建造（／东海群）分析为例,主张建立构造一建造综合分析思路;从抛射建造与月面相互作用的角度,提出并阐述了掘积系统的概念、掘积系统内外带之间划分的新标志即蚀积盂及其所组成的捩侵蚀带（TSZ）;在月球表面形貌构造区划分析的基础上,通过对月盆、月海的时空分布规律的分析、综合,提出月球晚期大轰击（LHB）所造成的月盆开掘期间,具有“轰击漂移”现象,并推测月球LHB过程中出现准对跖翻转;通过对古老月陆区所保存的线性构造解读和构造形迹的组合关系分析,尝试性地提出在冥月宙月球岩浆洋（LMO）演化晚期可能存在单板模式的月全球构造。月球构造演化从初始阶段的LMO所驱动的内动力体制转向冲击造成的外动力体制。     

上地幔熔体-岩石相互作用与大陆地幔演化

根据实验岩石学、幔源岩石的岩石地球化学资料以及微量元素地球化学理论模拟等,评述了上地幔熔体岩石相互作用研究领域的最新进展,指出熔体岩石相互作用不仅深刻地制约了岩石圈地幔的矿物学、地球化学和物理性质的变化以及地幔不均一性的形成及演化,而且也会最终控制各种构造环境下喷出岩浆的地球化学特征,以及深部岩浆的分离机制。     

上地幔熔体—岩石相互作用与大陆地幔演化

根据实验岩石学,幔源岩石的岩石地球化学资料以及微量元素地球化学理论模拟等,评述了上地幔熔体－岩石相互作用研究领域的最新进展,指出熔体－岩石相互作用不仅深刻地制约了岩石圈地幔的矿物学,地球化学和物理性质的变化以及地幔不均一性的形成及演化,而且也会最终控制各种构造环境下喷出岩浆的地球化学特征,以及深部岩浆的分离机制。     

大地构造火成岩岩石学研究

大地构造火成岩岩石学是岩石学和大地构造学研究相结合的学科,与传统的研究思路和方法相比,它重视深部地质过程的研究,尤其是大陆动力学的成就。通过深部物质信息（火成岩及包体、中高级变质岩）的研究,反演深部物质组成,为大地构造单元的划分对比提供深部证据;基性超基性构造岩浆带的研究是揭示古构造块体边界、超壳深大断裂的窗口;岩石圈组成的岩石学模型和垂向岩石圈分层界面的研究对于重新认识Ｍｏｈｏ面、低速层和大陆岩石圈结构意义重大。岩石学探针、同位素地球化学示踪和科学深钻、超深钻是现代大地构造火成岩岩石学研究的主要方法和手段。     

喜马拉雅造山带中新世岩浆型石榴子石的矿物化学特征:从高Sr/Y花岗岩到淡色花岗岩

石榴子石是演化花岗岩常见的重要副矿物之一,但石榴子石地球化学特征如何随岩浆演化而变化是有待探讨的问题之一。雅拉香波片麻岩穹隆发育年龄分别为20. 3±0. 5Ma和20. 1±0. 3Ma(锆石U-Pb年龄)的高Sr/Y比二云母花岗岩(TMG)和淡色花岗岩(Grt-LG)。虽然两类花岗岩都含石榴子石,且在形成时代和Sr-Nd同位素组成上相似,但在元素地球化学特征上具有明显的差异,淡色花岗岩和二云母花岗岩分别代表演化程度较高和较原始的岩浆。在同一件样品中,在石榴子石颗粒之间,存在一定程度的微量元素地球化学特征的不均一性,反映了局部熔体地球化学特征。在两类花岗岩中,岩浆型石榴子石具有以下相似的地球化学特征:(1)从核部到边部,Mn和HREE含量降低,表现出典型的生长环带特征;(2)富集HREE,亏损LREE;和(3)显著的Eu负异常。但在关键微量元素Zn、Sc和Y上,具有明显的差异性。在花岗质岩浆演化过程中,贫Fe、Mg和Mn矿物相的分离结晶作用,导致残留熔体的Ca和Sr含量降低,Eu负异常幅度增大,Sc、Zn、Y和HREE增高,是导致淡色花岗岩石榴子石相应元素含量增高的主要原因。上述观测表明:高Sr/Y花岗岩也可以结晶石榴子石,与通常的淡色花岗岩石榴子石相比,这些石榴子石的Sc、Zn和Y含量和Eu异常幅度明显较低。但随分异程度的升高,石榴子石的元素地球化学特征与源自变沉积岩的淡色花岗岩的类似。因此,花岗岩中的石榴子石矿物化学特征变化记录了花岗岩岩浆演化的重要信息。     

大别山碰撞后花岗岩锆石包裹物研究——对埃达克质岩源区及熔融深度的制约

大陆型埃达克岩的成因及其地质意义是一个很有争议的科学问题。大别地区发育有典型的加厚下地壳底部部分熔融产生的埃达克质岩。元素地球化学以及实验岩石学研究均表明,若这些埃达克质岩确来自加厚下地壳底部部分熔融,其残留相矿物应为石榴子石、绿辉石、金红石等高压矿物。本文对大别山埃达克质岩石和普通花岗岩中的锆石包裹物进行了激光拉曼光谱鉴定,证实了埃达克质岩中锆石存在石榴子石、绿辉石、金红石、白云母等矿物包裹物。如果这些矿物是与锆石在岩浆中共结晶形成的,这或可为大别山埃达克质岩的源区特征提供直接证据。     

Lunar Magma Ocean crystallization revisited: Bulk composition, early cumulate mineralogy, and the source regions of the highlands Mg-suite

Crystallization of the Lunar Magma Ocean (LMO) has been numerically modeled and its products inferred from sample observations, but it has never been fully tested experimentally. This study is a reexamination of the LMO hypothesis by means of the first experimental simulation of lunar differentiation. Two end-member bulk Moon compositions are considered: one enriched in refractory lithophile elements relative to Earth and one with no such enrichment. A “two-stage” model of magma ocean crystallization based on geophysical constraints is simulated and features early crystal suspension and equilibrium crystallization followed by fractional crystallization of the residual magma ocean. An initially entirely molten Moon is assumed. Part 1 of this study, presented here, focuses on stage 1 of this model and considers the early cumulates formed by equilibrium crystallization, differences in mantle mineralogy resulting from different bulk Moon compositions, and implications for the source regions of the highlands Mg-suite.Refractory element enriched bulk Moon compositions produce a deep mantle that contains garnet and trace Cr-spinel in addition to low-Ca pyroxene and olivine. In contrast, compositions without refractory element enrichment produce a deep dunitic mantle with low-Ca pyroxene but without an aluminous phase. The differences in bulk composition are magnified in the residual melt; the residual LMO from the refractory element enriched composition will likely produce plagioclase and ilmenite earlier and in greater quantities. Both compositions produce Mg-rich early cumulate piles that extend from the core-mantle boundary to ∼355 km depth, if 50% equilibrium crystallization and whole Moon melting are assumed. These early LMO cumulates provide good fits for the source regions for a component of the high-Mg^∗, Ni- and Co-poor parental magmas of the Mg-suite cumulates, if certain conditions are called upon. The olivine in early LMO cumulates produced by either bulk Moon composition is far too rich in Cr to be reasonable for the source regions of the Mg-suite, meaning either core formation in the presence of S and/or C must be invoked to deplete the LMO and the crystallizing olivine in Cr, or that current estimates of the bulk lunar Cr content are too high. We infer that melts meeting the criteria of the Mg-suite parents could be produced from early LMO cumulates by solid state KREEP and plagioclase hybridization near the base of the crust and subsequent partial melting. Additionally, we propose a revised model for Mg-suite petrogenesis.     

Inversion of the Main Mineral Compositions and Subdivision of Tectonic Units on Lunar LQ-4 based on Chang’e Data

Spectra are sensitive in detecting main minerals on the lunar surface from visible light to infrared light. Since spectral characteristics of minerals are closely related to their compositions and the maturity level of soil on the Moon, studying the compositions and distribution of elements and minerals on the lunar surface can help to understand the evolution of the Moon through remote sensing technology. The correlation between the spectral characteristics of Chang’e-1 interference imaging spectrometry (IIM) reflectance images and the mineral contents of LSCC (Lunar Soil Characterization Consortium) lunar surface mineral samples was discussed and the spatial distributions of FeO and Al2O3 contained in both pyroxene and plagioclase on LQ-4 were studied using the improved angle parameter method, MNF, and band ratio statistics. A comparison of the mapping results of the optical models by Lucey, Shkuractov and other researchers on Clementine and the gamma ray spectrometry data shows that the content error is within 0.6% for lunar mare areas and close to 1% for the highland areas. The tectonic framework on the lunar surface was also investigated. And based on integrated analysis of previous findings on topography of the lunar surface, Chang’e LAM, CCD and LOLA images and the gravity anomalies data (Clementine GLGM-2), the tectonic unit subdivision was established for LQ-4, the idea of subdividing the lunar tectonic units was proposed, and this will provide a good foundation for studying the lunar tectonic evolution.     

High-pressure phase transitions of anorthosite crust in the Earth's deep mantle

We investigated phase relations, mineral chemistry, and density of lunar highland anorthosite at conditions up to 125 GPa and 2000 K. We used a multi-anvil apparatus and a laser-heated diamond-anvil cell for this purpose. In-situ X-ray diffraction measurements at high pressures and composition analysis of recovered samples using an analytical transmission electron microscope showed that anorthosite consists of garnet, CaAl₄Si₂O₁₁-rich phase (CAS phase), and SiO₂ phases in the upper mantle and the mantle transition zone. Under lower mantle conditions, these minerals transform to the assemblage of bridgmanite, Ca-perovskite, corundum, stishovite, and calcium ferrite-type aluminous phase through the decomposition of garnet and CAS phase at around 700 km depth. Anorthosite has a higher density than PREM and pyrolite in the upper mantle, while its density becomes comparable or lower under lower mantle conditions. Our results suggest that ancient anorthosite crust subducted down to the deep mantle was likely to have accumulated at 660–720 km in depth without coming back to the Earth's surface. Some portions of the anorthosite crust might have circulated continuously in the Earth's deep interior by mantle convection and potentially subducted to the bottom of the lower mantle when carried within layers of dense basaltic rocks.     

Chemical composition of lunar meteorites and the lunar crust

The paper presents the first analyses of major and trace elements in 19 lunar meteorites newly found in Oman. These and literature data were used to assay the composition of highland, mare, and transitional (highland-mare interface) regions of the lunar surface. The databank used in the research comprises data on 44 meteorites weighing 11 kg in total, which likely represent 26 individual falls. Our data demonstrate that the lunar highland crust should be richer in Ca and Al but poorer in mafic and incompatible elements than it was thought based on studying lunar samples and the first orbital data. The Ir concentration in the highland crust and the analysis of lunar crater population suggest that most lunar impactites were formed by a single major impact event, which predetermined the geochemical characteristics of these rocks. Lunar mare regions should be dominated by low-Ti basalts, which are, however, enriched in LREEs compared to those sampled by lunar missions. The typical material of mare-highland interface zones can contain KREEP and magnesian VLT basalts. The composition of the lunar highland crust deduced from the chemistry of lunar meteorites does not contradict the model of the lunar magma ocean, but the average composition of lunar mare meteorites is inconsistent with this concept and suggests assimilation of KREEP material by basaltic magmas. The newly obtained evaluations of the composition of the highland crust confirm that the Moon can be enriched in refractory elements and depleted in volatile and siderophile elements.     

试论地球演化历史中水的总体行为

在地球不均匀吸积模型的基础上，根据比较行星学所获得的行星演化理论、大陆进化的历史、板块运动的特点以及高温高压实验研究结果，对地球演化历史中水的总体行为进行了分析和推论。从而对地球原始壳的特点、地球上液态水成因、地球表面缺失最初８亿年历史的原因、水的总体运移趋势等有了一些新的认识     

我国月球探测的总体科学目标与发展战略

在简述月球探测的历程与趋势的基础上,强调当代月球探测的总体目标为：①研究月球与地月系的起源和演化,特别是月球大气层与磁场的消失,矿物与岩石的分布和形成环境、月壤和内部层圈结构的形成以及月球演化的历程;②探测月球的资源、能源和特殊环境的开发利用及对人类社会长期可持续发展的支撑。我国不载人月球探测划分为绕、落、回三个阶段。为了全球性、整体性重新认识月球,绕月卫星探测的科学目标是为了获取全月面三维影像,探测14种有用元素的全球分布与丰度,探测月壤厚度并估算氦 3资源量以及太阳活动对空间环境的影响。"落"为月球探测器软着陆就位探测和月球车巡视探测,建立月基光学、低频射电和极紫外天文观测平台。"回"为月球探测器软着陆就位探测和取样返回地面。     

Lunar surface mineralogy using hyperspectral data: Implications for primordial crust in the Earth–Moon system

Mineralogy of the Lunar surface provides important clues for understanding the composition and evolution of the primordial crust in the Earth–Moon system. The primary rock forming minerals on the Moon such as pyroxene, olivine and plagioclase are potential tools to evaluate the Lunar Magma Ocean (LMO) hypothesis. Here we use the data from Moon Mineralogy Mapper (M³) onboard the Chandrayaan-1 project of India, which provides Visible/Near Infra Red (NIR) spectral data (hyperspectral data) of the Lunar surface to gain insights on the surface mineralogy. Band shaping and spectral profiling methods are used for identifying minerals in five sites: the Moscoviense basin, Orientale basin, Apollo basin, Wegener crater-highland, and Hertzsprung basin. The common presence of plagioclase in these sites is in conformity with the anorthositic composition of the Lunar crust. Pyroxenes, olivine and Fe-Mg-spinel from the sample sites indicate the presence of gabbroic and basaltic components. The compositional difference in pyroxenes suggests magmatic differentiation on the Lunar surface. Olivine contains OH/H₂O band, indicating hydrous phase in the primordial magmas.     

Volatile interactions with the lunar surface

The Moon is generally depleted in volatile elements and this depletion extends to the surface where the most abundant mineral, anorthite, features <6 ppm H₂O. Presumably the other nominally anhydrous minerals that dominate the mineral composition of the global surface—olivine and pyroxene—are similarly depleted in water and other volatiles. Thus the Moon is tabula rasa for the study of volatiles introduced in the wake of its origin. Since the formation of the last major basin (Orientale), volatiles from the solar wind, from impactors of all sizes, and from volatiles expelled from the interior during volcanic eruptions have all interacted with the lunar surface, leaving a volatile record that can be used to understand the processes that enable processing, transport, sequestration, and loss of volatiles from the lunar system. Recent discoveries have shown the lunar system to be complex, featuring emerging recognition of chemistry unanticipated from the Apollo era, confounding issues regarding transport of volatiles to the lunar poles, the role of the lunar regolith as a sink for volatiles, and the potential for active volatile dynamics in the polar cold traps. While much has been learned since the overturn of the “Moon is dry” paradigm by innovative sample and spacecraft measurements, the data point to a more complex lunar volatile environment than is currently perceived.