天山石炭-二叠纪大火成岩省裂谷火山作用与地幔柱

中国西北部石炭纪-早二叠世喷发的天山裂谷火山岩系构成了一个大火成岩省。该火山岩系的组成以玄武质熔岩为主，其次有中性和酸性熔岩及火山碎屑岩。根据岩石学、主元素、微量元素和Sr—Nd—Pb同位素数据，天山玄武岩可分为两个主要岩浆类型：①高Ti／Y（HT）类型，以高Ti／Y（〉500）、高Ce／Y（〉3）和相对低Nb／Zr（〈0．11）、低εNd（t）为特征；②低Ti／Y（LT）类型，以低Ti／Y（〈500）为特征。LT熔岩又可以进一步分为两个亚类：LT1熔岩以低Nb／Zr（〈0．15）和高εNd（t）（＋3．1～＋9．7）为特征；LT2熔岩具有较高的Nb／Zr值（〉0．16）和较低的εNd（t）值（-0．98～-2．91）。元素和同位素数据表明，HT和LT熔岩的化学变异不是由一个共同母岩浆的结晶分异作用所产生。它们极有可能是源于一种似洋岛玄武岩源的幔源（^87St／^86Sr（t）≈0．7045，εNd（t）≈＋4，^206Pb／^204Pb（t）≈18．35．^207Pb／^204Pb（t）≈15．66，^208Pb／^204Pb（t）≈38．25．La／Nb≈0．7），且具有不同的熔融条件和经受了不同的分异和混染。以碱性熔岩为主的HT熔岩是产生于幔源石榴子石稳定区的低度部分熔融，其化学变异受控于单斜辉石（Cpx）[士橄榄石（O1）]分离作用。相反，LT类型的母岩浆则是形成于幔源的尖晶石一石榴子石过渡带：碱性LT2亚类的母岩浆是产生于部分熔融程度较低的条件下；而以拉斑玄武质为主的LT1亚类的母岩浆则是产生于部分熔融条件较高的条件下：它们经受了浅层辉长岩质分离作用，化学变异较大。天山玄武岩可能是产生于地幔柱头。HT和LT岩浆的岩石成因又进一步为地壳和岩石圈地幔的混染作用所复杂化。我们的研究揭示，天山大火成岩省的火山岩中存在空间上的岩石地球化学变化。天山东段的LT1火山岩系的厚度最大．它们记录了玄武岩侵位的主幕，该处可能是地幔柱或地幔熔融异常的中心位置。相反，厚度较小的HT和LT2玄武岩则可能是意味着地幔柱活动影响的减弱。事实上，HT和LT2玄武岩也是该大火成岩省边缘部分的主要岩浆类型。HT和LT2熔岩的地幔熔融程度较低，可能是与地幔柱边部的岩石圈相对较厚和地热较低有关。     

内蒙古集宁新生代玄武岩的地幔源区特征：元素及Sr-Nd-Pb同位素地球化学证据

内蒙古集宁玄武岩区位于华北克拉通北缘，东邻汉诺坝玄武岩区。由亚碱性的拉斑玄武岩及碱性的橄榄玄武岩、碧玄岩和碱玄岩组成。玄武岩的SiO2与TiO2含量分别为44．10～52．27wt．％和1．57～2．95wt．％，Mg^#（43—63）及Ni含量（27～210ppm）变化范围较大。集宁玄武岩的微量元素原始地幔标准化曲线及REE球粒陨石标准化曲线与OIB相似，Sr、Nd同位素比值显示了较汉诺坝玄武岩富集的特征。研究表明，虽然集宁玄武岩浆经历了一定程度的橄榄石、单斜辉石的分离结晶作用，但微量元素及Sr、Nd、Ph同位素特征排除了幔源岩浆在喷发到地表过程中受到地壳物质显著混染的可能性。^143Nd／^144 Nd ^87Sr／^86Sr vs．^206Ph／^204Pb的线性相关性表明，集宁玄武岩至少来自两个地幔端元组分：EMI和PREMA，且端元组分与汉诺坝玄武岩相似。尖晶石二辉橄榄岩的低程度部分熔融（2～5％）熔体与石榴石二辉橄榄岩更低程度部分熔融（〈2％）熔体的混合，可以解释集宁玄武岩稀土元素的变化特征。推测EMI位于岩石圈地幔之内且源区深度〈70km，PREMA则来自软流圈地幔。集宁碱性玄武岩与亚碱性玄武岩之间的地球化学差异，可能只是来自岩石圈地幔的EMI型熔体和来自软流圈地幔的PREMA型熔体在形成玄武岩浆时参与混合的比例不同，暗示该地区的岩石圈地幔与软流圈地幔之间经历了强烈的相互作用。集宁玄武岩与汉诺坝玄武岩相似的Sr、Nd、Pb同位素比值及相关性，说明它们具有相似的地幔源区，汉诺坝玄武岩的地球化学差异同样可以用EMI与PREMA组分对岩浆贡献程度的不同来解释。     

新疆三塘湖盆地古生代晚期火山岩地球化学特征及其构造-岩浆演化意义

三塘湖盆地早石炭世安山岩（ECA）、早二叠世粗面岩类（EPT）以及中二叠世玄武岩（MPB）样品都具有大离子亲石元素（LILE）相对于高场强元素（HFSE）富集，Nb和Ta强烈亏损，轻稀土元素（LREE）相对于重稀土元素（HREE）富集，类似于和俯冲带相关的岩浆特征。ECA具有高的Zr／Nb（4．67～12．39），低的Nb／La（0．27～0．30），Ce／Ce＊=0．63～0．89，Sr／Sr＊=1．32．2．49，并具有Ti的负异常，另外（^87Sr／^86Sr）i=0．70408～0．70451，εNd（t）=＋7．42-＋7．88。与ECA相比，EPT大离子亲石元素更为富集，Ti和P的负异常明显，特别是Ce／Ce＊=0．72—1．64，Sr／Sr＊=0．38～1．87，相对较低的Al2O3和CaO含量以及（^87Sr／^86Sr）；=0．70414～0.70481和εNd（t）=＋4．93～＋6．13而区别于ECA。MPB与ECA相比具有较低的大离子亲石元素含量和较高的Nb、Ta含量，Ce／Ce＊=0．69～0．84，Sr／Sr＊=1、44～2．13，未有明显的Ti负异常，（^87St／^86Sr）i=0．70388～0．70396，εNd（t）=＋7．10-＋7．99。所有的地球化学特征表明：早石炭世或更早，三塘湖盆地为与俯冲带相关的构造背景，ECA是典型的弧火山岩，其岩浆主要源于被流体或沉积物交待改造的亏损地幔楔。早石炭世以后，三塘湖地区逐渐进入碰撞后伸展拉张阶段，EPT和MPB都为后造山火山岩。EPT岩浆主要源于亏损软流圈底侵前二叠纪形成的造山组分的部分熔融；MPB的岩浆主要源于亏损地幔的部分熔融，并被前二叠纪形成的造山组分或是年轻地壳混染。三塘湖地区二叠纪伸展拉张的动力学机制主要是由于造山带增厚的岩石圈大范围拆沉而导致的大范围亏损地幔部分熔融岩浆和上部造山组分或是年轻地壳的相互作用，这种造山组分或是年轻地壳具有低的（^87Sr／^86Sr），比值和正的εNd（t）值。火山岩地球化学特征指示没有明显地幔柱的作用特征。     

南秦岭中段西乡群火山岩岩石成因

南秦岭中段新元古代中期（730-845Ma）西乡群（自下而上包括孙家河组、大石沟组和白勉峡组）火山岩喷发于大陆板内裂谷环境。它们极有可能与导致Rodinia超大陆裂谷化裂解的地幔柱活动有关。根据岩石地球化学数据．南秦岭中段新元古代中期西乡群裂谷基性熔岩总体上属于低Ti／Y（LT,Ti／Y〈500）岩浆类型。LT熔岩又可进一步划分为LT1和LT2等2个亚类。LT1熔岩以高Nb／La（0．87～0．98）、低Thw／NbN（≈1）、缺乏Nb—Ta和Ti的亏损、具有“大隆起”式微量元素原始地幔标准化分配型式、（^87SrSr^86Sr）（t）=0．703869、εNd（t）=4．83为特征,属于拉斑玄武质岩浆系列;LT2熔岩以低Nb／La（〈0．75）、高ThN／NbN（〉1．4）、Nb—Ta和Ti亏损明显和Sr—Nd同位索比值变化较大为特征。元素和同位素数据表明,西乡群裂谷火山岩的化学变化不是由一个共同的母岩浆结晶分异作用所产生。孙家河组、大石沟组和自勉峡组中TiO2含量大于1．09％的火山岩的母岩浆经受了辉长岩质结晶分离作用。而白勉峡组中TiO2含量小于0．69％的基性熔岩的化学演化则是受控于单斜辉石（cpx）±橄榄石（ol）结晶分离作用。西乡群火山岩系中,基性、中性和酸性熔岩间为分异结晶关系。南秦岭中段新元古代中期西乡群裂谷火山岩系极有可能是源于共同的地幔柱,该地幔柱组分的成分为;εNd（t）≈＋5,^87Sr／^86Sr（t）≈0．704,La／Nb≈0．7。南秦岭中段新元古代中期西乡群裂谷基性熔岩存在空间上的地球化学变化：LT1熔岩的母岩浆,没有受到明显的大陆岩石圈混染,保存了鲜明的地幔柱信号;而大陆地壳或大陆岩石圈混染作用对于LT2熔岩的形成则有着重要贡献。研究揭示,南秦岭中段新元古代中期西乡群裂谷基性熔岩的母岩浆总体上产生于上涌地幔柱上部层位（地幔柱头）3GPa?     

胶莱盆地晚白垩世不同地幔源区的两种基性岩浆——诸城玄武岩和胶州玄武岩的对比

采用全岩K-Ar法获得山东省胶莱盆地诸城玄武岩的形成年龄为76M，胶州玄武岩的形成年龄为72Ma，代表了发生在晚白垩世的地幔岩浆事件，但两地岩浆产物具有不同的地球化学性质。诸城玄武岩主要为粗面玄武岩，富集轻稀土元素（LREE），微量元素组成类似于洋岛玄武岩（OIB），（^87Sr/^86Sr）t=0．7060-0．7080，εNd（t）=-3．0--5．1，介于洋岛玄武岩和中生代富集的岩石圈地幔之间，表明软流圈来源的岩浆中混入了富集岩石圈地幔来源的岩浆，是软流圈地幔与岩石圈地幔相互作用的结果。胶州玄武岩主要为碱性玄武岩，比诸城玄武岩更富集轻稀土元素，微量元素组成类似于诸城玄武岩，但Nb、Ta、Ti等高场强元素不显示亏损，Sr-Nd同位素组成也存在明显差别，（^87Sr/^86Sr）t=0、70350-0．70355，εNd（t）=5．4-5．8，与山东省新生代火山岩的地球化学特征类似，类似于洋岛玄武岩（OIB），表明岩浆起源于亏损的软流圈地幔。研究显示出晚白垩世以来胶莱盆地软流圈地幔不均匀上涌和逐渐成为玄武岩浆主要源区的趋势。     

壳幔作用导致武平花岗岩形成——Sr-Nd-Hf-U-Pb同位素证据

岩石学、元素地球化学和Sr-Nd-Hf-U-Pb同位素的综合研究显示,武平花岗质杂岩体是由形成时代和成因不同的黑云母花岗岩和含石榴子石花岗岩组成。LA-ICPMS锆石U-Pb定年指示前者形成于161．4 Ma,后者形成于113 Ma。黑云母花岗岩以中等富集大多数不相容元素和中等轻重稀土分异为特征,岩石具有低的87Sr／86Sr初始比值(<0．710)和高的εNd(t) 值(-2．6--5．7)。结合与附近基底变质岩的同位素对比,论文指出黑云母花岗岩岩浆是由元古代基底变质岩部分熔融产生的熔体与幔源岩浆的强烈混合形成。不均匀的锆石Hf同位素组成(εHf(t)=-3．6--10．8)支持了这种混合成因模式。含石榴子石花岗岩以富Si、Al、Na、K、Nb、Ta、Y和HREE而贫P、Sr、Ba、LREE、Zr和Hf含量为特征,它们具有低的(La/Yb)n, Zr／Hf、Nb／Ta比值和高的Rb／Sr比值,显示了强烈的以斜长石为主的分异特征;它们的87Sr／86Sr初始比值大于0．710,εNd(t) =-7．1,锆石的Hf同位素较低且相对均匀(εHf(t)平均值为-9．7),表明岩浆没有受到明显的地幔组分混染。结合它们高的HREE含量,论文指出它们的母岩浆很可能是由早期熔融事件的富石榴子石残留相再次熔融形成。因此,南岭地区中生代花岗岩的地球化学差异很可能反映了岩浆形成过程中壳幔作用的强弱。     

长江中下游繁昌盆地火山岩年代学和地球化学:岩石成因和地质意义

长江中下游地区发育多个中生代火山盆地,自西向东依次为金牛、怀宁、庐枞、繁昌、宁芜、溧水和溧阳盆地.繁昌盆地自下而上发育中分村组、赤沙组和蝌蚪山组火山岩.中分村组下段和上段流纹岩的LA-ICPMS锆石U-Pb定年结果分别为131.2±1.1Ma和129.1±1.3Ma,和蝌蚪山组流纹岩的形成时代(130.7±1.1Ma)在误差范围内一致,表明繁昌盆地火山岩喷发持续时间较短.中分村组发育英安岩和流纹岩,赤沙组以粗安岩为主,并有少量的流纹岩,两者的SiO2含量分别为64.36％ ～75.45％和63.08％ ～69.75％.中分村组和赤沙组火山岩的稀土和微量元素特征基本一致,均富集轻稀土和大离子亲石元素,亏损Nd、P和Ti,其中,流纹岩表现为Eu的负异常.中分村组样品的87Sr/86 Sr(t)为0.7060 ～ 0.7074,εNd(t)为-7.91～ -8.11,赤沙组样品的87Sr/86Sr(t)为0.7073,εNd(t)为-6.62～ -6.71,和蝌蚪山组玄武岩的Sr-Nd同位素组成很相似.综合分析表明,中分村组火山岩为岩石圈地幔部分熔融的岩浆底侵形成的下地壳再次部分熔融的产物,并经过辉石、角闪石、斜长石和磷灰石的结晶分异.赤沙组粗安岩为岩石圈地幔部分熔融形成的玄武岩浆,经过橄榄石、辉石、斜长石和钛铁氧化物结晶分异形成.岩石圈地幔的部分熔融在长江中下游地区中生代火山岩中表现的最为集中,表明～ 130Ma时期为本地区的拉张峰期.     

西天山阿吾拉勒埃达克质岩石成因：Nd和Sr同位素组成的限制

西天山阿吾拉勒二叠纪钠质英安岩和钠长斑岩具有与埃达克岩一致的高Sr,低Y、Yb和Eu正异常等独特岩石地球化学特征。系统的Nd和Sr同位素组成研究表明，其（^143Nd/^144Nd)i为0．512384－0．512470，εNd(t)为正值（＋1．57－＋3．26）；（^87Sr/^86Sr)i为0．0751－0．7054，与本区同时代幔源玄武岩的Nd和Sr同位素组成特征相似，但与俯冲洋壳部分熔融成因埃达克岩的Nd和Sr同位素组成有显著区别。结合这些埃达克质岩石形成二叠纪后碰撞阶段构造背景，认为本区埃达克质岩浆最有可能由新底侵的玄武质下地壳在角闪岩相向榴辉岩相过渡或榴辉岩相的条件下部分熔融形成，是西天山晚古生代后碰撞阶段地幔玄武岩浆底侵作用和地壳垂向增生的重要岩石标志。     

峨眉地幔柱-岩石圈的相互作用:来自低钛和高钛玄武岩的Sr-Nd和O同位素证据

蛾眉山玄武岩总体具有较高的^87Sr／^86Sr比值和较低的εNd(t)值，并具有富集地幔源区的特点。而低钛玄武岩(LT)与高钛玄武岩(HT)间又表现出一定的差异性，即早期低钛玄武岩(LTl)的^87Sr/^86Sr比值最高(0．7063—0．7078)，而其εNd(t)最低(—6．74-—0．34)：晚期高钛玄武岩(HT)具有最低的^87Sr/^86Sr比值(0．7049—0．7064)和最高的εNd(t)值(—0．71—1．5)。蛾眉山低钛玄武岩中单斜辉石的氧同位素变化范围为6．2‰-7．86‰，高于洋岛拉斑玄武岩的平均值5．4‰。研究样品较地幔岩石偏高的δ^18O值说明在其形成和演化过程中有壳源物质的参与。结合前人的研究成果和对元素地球化学的研究认为，壳源物质可能主要来自于新元古代富集的扬子西缘次大陆岩石圈地幔。地幔柱—岩石圈的相互作用过程中表现在时间和空间的系统变化，即早期西岩区形成含大量壳源组分的低钛玄武岩，晚期为壳源组分相对较少的高钛玄武岩。空间上低钛玄武岩仅分布在西岩区，而中、东岩区皆为高钛玄武岩。壳源组分随着时间演化逐渐减少，在空间上由西而东也逐渐减少。表明蛾眉山火成岩省形成早(主)期地幔柱头卷入并熔融了较多交代富集的次大陆岩石圈物质，晚期则有较少的壳源物质参与。建立了蛾眉地幔柱与大陆岩石圈作用的工作模型。     

粤西阳春中生代钾玄质侵入岩及其构造意义：

粤西阳春地区马山二长闪长岩强烈富集K、Sr和LREE，(87Sr／86Sr)；≈0.7046，εNd(t)≈+1；岗尾-轮水岩体较富集K、Rb、Th和LREE，(87Sr／86Sr)：≈0.7063，εNd(t)≈-2；石岩体较富集Sr，K、Rb、Th和LREE相对较低，(87Sr／86Sr);=0.7084～0.7089，εNd(t)≈-6。马山岩体来源于大离子亲石元素(ULE)和LREE富集的交代地幔；岗尾-轮水岩体来自于放射成因Sr、Nd同位素组成略高或交代时间略早的富集交代地幔，并且经历了明显的结晶分异作用；石岩体则很可能是前存下地壳底垫基性岩重熔形成的。从早侏罗世到早白垩世，南岭西部的岩浆成分和源区的规律性变化反映了区域软流圈地幔上涌和岩石圈伸展-拉张-减薄的演化过程。     

月球火山碎屑堆积物光谱研究

月球的火山作用是月球的重要内生地质过程,反映了月球的内部演化。由爆发式火山作用形成的月球火山碎屑堆积物（LPD）代表了比月海玄武岩更深部的物质,是月球探测的优先目标之一。反射光谱是研究月球火山碎屑堆积物、在全球尺度上区分月球爆发式火山与溢流式火山的重要手段。文中选取29个已经确认的火山碎屑堆积物并结合模拟月球玻璃样品开展光谱学研究,建立了富玻璃的LPD光谱识别指标。根据模拟月球玻璃的铁钛含量与其1 μm处吸收特征的关系比较了富玻璃火山碎屑堆积的相对铁钛含量,为今后提高月球火山碎屑堆积物的铁钛反演精度提供思路。研究结果表明,在这29个火山碎屑堆积中,Sulpicius Gallus、Gauss、Walther A、Birt E和Aristarchus是较为富玻璃的火山碎屑堆积。Aristarchus、Sulpicius Gallus和Birt E的钛含量低于Walther A、Gauss,Birt E, 1 μm左吸收肩偏短波方向,1 μm吸收深度较浅,这可能因为Birt E具有异常低的Fe含量,或者其光学成熟度较高。鉴于火山碎屑堆积物重要意义,其是未来月球采样的较佳候选地区。     

A laser-ablation ICP-MS study of Apollo 15 low-titanium olivine-normative and quartz-normative mare basalts

Apollo 15 low-Ti mare basalts have traditionally been subdivided into olivine- and quartz-normative basalt types, based on their different SiO₂, FeO, and TiO₂ whole-rock compositions. Previous studies have reconciled this compositional diversity by considering the olivine- and quartz-normative basalts as originating from different lunar mantle source regions. To provide new information on the compositions of Apollo 15 low-Ti mare basalt parental magmas, we report a study of major and trace-element compositions of whole rocks, pyroxenes, and other phases in the olivine-normative basalts 15016 and 15555 and quartz-normative basalts 15475 and 15499. Results show similar rare-earth-element patterns in pyroxenes from all four basalts. The estimated equilibrium parental-melt compositions from the trace-element compositions of pyroxenes are similar for 15016, 15555 and 15499. Additionally, an independent set of trace-element distribution coefficients has been determined from measured pyroxene and mesostasis compositions in sample 15499. These data suggest that fractional crystallization may be a viable alternative to compositional differences in the mantle source to explain the 25% difference in whole-rock TiO₂, and corresponding differences in SiO₂ and FeO between the Apollo 15 olivine- and quartz-normative basalts. In this model, the older (3.35 Ga) quartz-normative basalts, with lower TiO₂ experienced olivine, chromite, and Cr-ulvöspinel fractionation at ‘crustal levels’ in magma chambers or dikes, followed by limited near-surface mineral fractionation, within the lava flows. In contrast, the younger (3.25 Ga) olivine-normative basalts experienced only limited magmatic differentiation at ‘crustal-levels’, but extensive near-surface mineral fractionation to produce their evolved mineral compositions. A two-stage mineral-fractionation model is consistent with textural and mineralogical observations, as well as the mineral trace-element constraints developed by this study.     

Comparative petrology, geochemistry, and petrogenesis of evolved, low-Ti lunar mare basalt meteorites from the LaPaz Icefield, Antarctica

New data is presented for five evolved, low-Ti lunar mare basalt meteorites from the LaPaz Icefield, Antarctica, LAP 02205, LAP 02224, LAP 02226, LAP 02436, and LAP 03632. These basalts have nearly identical mineralogies, textures, and geochemical compositions, and are therefore considered to be paired. The LaPaz basalts contain olivine (Fo_64-2) and pyroxene (Fs₃₂Wo₈En₆₀ to Fs_84-86Wo₁₅En_2-0) crystals that record extreme chemical fractionation to Fe-enrichment at the rims, and evidence for silicate liquid immiscibility and incompatible element enrichment in the mesostasis. The basalts also contain FeNi metals with unusually high Co and Ni contents, similar to some Apollo 12 basalts, and a single-phase network of melt veins and fusion crusts. The fusion crust has similar chemical characteristics to the whole rock for the LaPaz basalts, whereas the melt veins represent localized melting of the basalt and have an endogenous origin. The crystallization conditions and evolved nature of the LaPaz basalts are consistent with fractionation of olivine and chromite from a parental liquid similar in composition to some olivine-phyric Apollo 12 and Apollo 15 basalts or lunar low-Ti pyroclastic glasses. However, the young reported ages for the LaPaz mare basalts (∼2.9 Ga) and their relative incompatible element enrichment compared to Apollo mare basalts and pyroclastic glasses indicate they cannot be directly related. Instead, the LaPaz mare basalts may represent fractionated melts from a magmatic system fed by similar degrees of partial melting of a mantle source similar to that of the low-Ti Apollo mare basalts or pyroclastic glasses, but which possessed greater incompatible element enrichment. Despite textural differences, the LaPaz basalts and mare basalt meteorite NWA 032 have similar ages and compositions and may originate from the same magmatic system on the Moon.     

峨眉山大火成岩省“高钛玄武岩”和“低钛玄武岩”成因探讨

大量的岩石化学资料分析表明，峨眉山大火成岩省玄武岩的TiO2含量是连续变化的，不存在明显的间断。野外地质特征表明高钛和低钛玄武岩既不存在空间分带，也不存在时间分带。其Sr、Nd和Pb同位素组成也没有明显的区别，推测它们可能是同源岩浆分离结晶的产物。根据MgO和TiO2的相关关系，可将苦橄岩和玄武岩的演化划分为4个趋势，并采用分离结晶模式对其进行了成因模拟，表明高钛和低钛玄武岩是同—母岩浆(苦橄—玄武岩浆)通过不同矿物相分离结晶的产物。     

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。     

Basalts as probes of planetary interiors: Constraints on the chemistry and mineralogy of their source regions

Basalt magmas, derived by the partial melting of planetary interiors, have compositions that reflect the pre-accretionary history of the material from which the planet formed, the planets, subsequent evolutionary history, the chemistry and mineralogy of the source regions, and the intensive thermodynamic parameters operating at the source and emplacement sites. Studies of basalt suites from the Earth, its Moon, and the eucrite parent body reveal compositional differences intrinsic to their source regions which are, in turn, a characteristic of the planet and its formational and evolutionary history.Major interplanetary differences are observed in iron, , TiO₂, Al₂O₃, Na₂O, Cr, Ni, and in volatile element abundances. The most primitive mare basalts have Mg#s 0.6, on the Earth they are 0.70–0.72 for mid-ocean ridge basalts (MORBs) and up to 0.9 for Archean peridotitic komatiites. Eucrites have Mg#s approaching 0.5 (excepting Binda). These differences reflect inherent differences in of their sources. Striking differences in the TiO₂ abundances of the planetary basalts reflect both inter- and intra-planetary variations in source chemistry. Primitive MORBs and primitive oceanic intraplate tholeiites have a factor of 2–3 difference in TiO₂ at comparable Mg# (0.7–1.2 vs 2–3 wt.% respectively). Three major titania groups are recognized in the mare suite; high TiO₂ (8–13 wt.%), low TiO₂ (2–5 wt.%) and very low TiO₂ (<1 wt.%). The eucrites have TiO₂ contents <1 wt.%.The mare basalts and eucrites have pronounced Na₂O depletion relative to all terrestrial basalts. This is a consequence of the preplanetary accretion loss of volatiles from the material that formed the Moon and the eucrite parent bodies.Mare basalts have consistently lower Al₂O₃ contents than the terrestrial basalts. This may be due either to an inherently lower content of Al₂O₃ in the mare sources or it may reflect Al₂O₃ retention in an aluminous phase.The transition metals are fractionated in all three basalt suites. For terrestrial basalts this may reflect core-separation; however, in the case of the Moon and eucrite parent bodies pre-accretionary separation of metal and silicates is a more reasonable explanation. A pronounced Cr anomaly is observed in terrestrial MORBs but not in the mare basalts. This appears to be related to f_O2 differences in the respective mantles.Overall rare earth element abundances are comparable between all three objects. Mare basalts have a pronounced negative Eu anomaly which is inherited from their source region and is record of plagioclase removal from crystallizing magma ocean early in lunar history (4.4–4.6 Ga). Early separation of plagioclase on the Earth appears to have been a relatively unimportant process.     

Basaltic magmatism on the Moon: A perspective from volcanic picritic glass beads

It is widely accepted that basaltic magmas are products of partial fusion of periodotite within planetary mantles. As such, they provide valuable insights into the composition, structure, and processes of planetary interiors. Those compositions which approach primary melt compositions provide the most direct information about planetary interiors and serve as a starting point to understand basaltic evolution. Within the collection of lunar samples returned by the Apollo and Luna missions are homogeneous, picritic glass beads of volcanic origin. These picritic glasses are our closest approximations to primary magmas. As such, these glass beads provide a unique perspective concerning the origin of mare basalts, the characteristics of the lunar interior, and processes in the early differentiation of the Moon. We have obtained trace element data for these picritic glasses using SIMS techniques. These data and literature isotopic and experimental data on the picritic glasses are placed within the framework of mare basaltic magmatism.The volcanic glasses are very diverse in their trace element characteristics, for example, they have a wide range of REE pattern shapes and concentrations. Like the crystalline mare basalts, all picritic glasses have a negative Eu anomaly. Unlike the crystalline mare basalts, there is little correlation between the size of the Eu anomaly and overall REE concentrations. Trace element differences among the various glasses suggests that a KREEP component was incorporated into their mantle source. This implies large scale mixing of the “Lunar Magma Ocean”-derived cumulate pile. Subtle differences among glasses suggest that local mixing of sources may also have been an important process. Preservation of subtle chemical differences in the picritic glasses and crystalline basalts may be interpreted as indicating that they were produced by small to moderate degrees of partial melting and that the lunar mantle did not experience extensive melting during episodes of mare volcanism.Several lines of evidence are consistent with the view that the picritic glasses were derived from mantle sources that were compositionally distinct from the sources for crystalline mare basalts. These are parallel, but no common, liquid lines of descent; chemical differences between picritic glasses and the more primitive crystalline mare basalts; experimental studies indicating that the picritic glasses are multiply saturated at depths greater than that of the mare basalts; differences in lead isotopic data; and the mode of eruption (i.e., fire fountaining for glass beads). These data also provide circumstantial evidence that suggests that the picritic glasses were derived from a source somewhat more volatile-rich than that of the mare basalts.Several petrogenetic models are suggested by the trace element characteristics of the picritic glasses:

• 1.(1) Partial melting of heterogeneous lunar mantle at depths greater than 300 km to produce the parental magmas (picritic) for both the mare basalts and picritic glasses. Picritic magmas represented by glass beads were erupted to the surface with small degrees of fractional crystallization while mare basalts were produced by larger degrees of fractional crystallization (15–30%) of similar (but not identical) picritic magmas.
• 2.(2) Picritic magmas represented by the glass beads were generated at depths greater than 400 km in a volatile-enriched (relative to the mare basalt source) heterogeneous mantle while mare basalts are fractional crystallization products of picritic magmas generated at depths of less than 400 km.
• 3.(3) The picritic magmas represented by the glass beads represent polybaric melting that initiated at depths of at least 1000 km. A primitive mantle component or less processed cumulate mantle components may have been involved in the generation of the picritic glasses in any of these models.

     

Antarctic lunar meteorites Yamato-793169, Asuka-881757, MIL 05035, and MET 01210 (YAMM): Launch pairing and possible cryptomare origin

The Antarctic lunar meteorite Meteorite Hills (MET) 01210 is a polymict regolith breccia, dominantly composed of mare basalt components. One relatively large (2.7 × 4.7 mm) basalt clast in MET 01210 (MET basalt) shows remarkable mineralogical similarities to the lunar-meteorite crystalline mare basalts Yamato (Y)-793169, Asuka (A)-881757, and Miller Range (MIL) 05035. All four basalts have similar rock texture, mineral assemblage, mineral composition, pyroxene crystallization trend, and pyroxene exsolution lamellae. The estimated TiO₂ contents (∼2.0 wt%) of the MET basalt and MIL 05035 are close to the bulk-rock TiO₂ contents of Y-793169 and A-881757. These similarities suggest that Y-793169, A-881757, MIL 05035, and the MET basalt came from the same basalt flow, which we designate the YAMM basalt. The source-basalt pairing of the YAMM is also supported by their similar REE abundances, crystallization ages (approx. 3.8-3.9 Ga), and isotopic compositions (low U/Pb, low Rb/Sr, and high Sm/Nd). The pyroxene exsolution lamellae, which are unusually coarse (up to a few microns) by mare standards, imply a relatively slow cooling in an unusually thick lava and/or subsequent annealing within a cryptomare. Reported noble gas and CRE data with close launch ages (∼1 Ma) and ejection depths (deeper than several meters) among the four meteorites further indicate their simultaneous ejection from the moon. Despite the marginally close terrestrial ages, pairing in the conventional Earth-entry sense seems unlikely because of the remote recovery sites among the YAMM meteorites.The high abundance (68%) of mare components in MET 01210 estimated from a two-component mixing model calculation could have resulted from either lateral mixing at a mare-highland boundary or vertical mixing in a cryptomare. The proportion of mare materials in MET 01210 is greater than in Apollo core samples at the mare-highland boundary. The burial depth (>several meters deep) inferred from the lack of surface irradiation of MET 01210 exceeds the typical mare regolith thickness (a few meters). Thus, the source of the YAMM meteorites is likely a terrain of locally high mare-highland mixing within a cryptomare. We searched for a possible source crater of the YAMM meteorites within the well-defined cryptomare, based on the multiple constraints obtained from this study and published data. An unnamed 1.4 km-diameter crater (53°W, 44.5°S) on the floor of the Schickard crater is the most suitable source for the YAMM meteorites.The ²³⁸U/²⁰⁴Pb (μ) value of the YAMM basalts is extremely low, relative to those of the Apollo mare basalts, but comparable to those of the Luna 24 very low-Ti basalts. The low-μ source indicates a derivation from a less differentiated mantle with a lack of KREEP components. Although the chemical sources of materials and heat source of melting might be independent, the heat source that generated the source magma of the YAMM and Luna 24 basalts may not be related to KREEP, unlike the case of the Apollo basalts. The distinct chemical and isotopic compositions of mantle sources between the Apollo basalts and the YAMM/Lunar 24 basalts imply differences in mantle composition and thermal evolution between the Procellarum KREEP Terrane (PKT) and non-PKT regions of the nearside.     

Petrology and geochemistry of LaPaz Icefield 02205: A new unique low-Ti mare-basalt meteorite

LaPaz Icefield 02205 (LAP 02205) is a new low-Ti mare-basalt meteorite that was discovered in the LaPaz Ice Field in Antarctica. This is the first crystalline lunar basalt in the US Antarctic collection and the only 5th unbrecciated mare-basalt meteorite to be discovered to date. The rock has a typical basaltic texture with tabular and elongated pyroxene and plagioclase crystals, and minor olivine grains commonly rimmed by pyroxenes. Core- to rim-zoning in terms of Fe and Mg is present in almost all pyroxene grains. Accessory minerals include ilmenite, chromite, ulvöspinel, troilite, and FeNi metal. This rock is highly enriched in late-stage mesostasis. Free silica is also abundant. In terms of texture and mineralogy, LAP 02205 displays features of low-Ti mare basalts, with similarities to some low-Ti Apollo 12 and Apollo 15 basalts. Whole-rock major- and trace-element compositions confirm the highly fractionated nature of this basalt. The whole-rock REE contents of the meteorite are the highest among all known low-Ti mare basalts. The platinum group element (PGE) contents in LAP are also enriched suggesting the possibility of endogenously enriched source regions or the PGEs generally behaved as incompatible elements during crystal fractionation under low fO₂ conditions. Trace-element contents of mineral grains in LAP 02205 display wide variations, suggesting extensive non-equilibrium crystallization. The REE concentrations in the earliest-formed minerals provide constraints on the composition of the parental liquid, which is similar to the measured whole-rock composition. Crystallization modeling of the LAP 02205 bulk composition yields a reasonable fit between predicted and observed mineral phases and compositions, except for the high-Mg olivine cores, which are observed in the rock but not predicted by the modeling. An isochron age of 2929 ± 150 Ma for phosphate minerals makes this rock one of the youngest lunar basalts known to date. The young age and specific geochemical characteristics of LAP distinguish it from those of most other low-Ti mare basalts. However, the low-Ti mare basalt meteorite, NWA 032, has a similar young age, and the two meteorites also appear to be closely related from some geochemical perspectives and might have originated from similar source regions on the Moon.     

嫦娥一号干涉成像光谱仪数据再校正与全月铁钛元素反演

月球表面的元素和物质成分分布是理解月球成岩与地质演化历史的重要线索。嫦娥一号干涉成像光谱仪(IIM)是我国首台月球探测成像光谱仪器,其获得的大量月球高光谱数据已成为我国未来探测月球成分与地质演化研究的宝贵基础数据。本文利用探月工程地面应用系统发布的IIM B版本2C级数据,开发出一套数据再定标流程,获得了较为可靠的月表相对反射率数据。我们在新校正数据的基础上开展月球表面FeO、TiO_2的反演建模,获得了全月FeO和TiO_2分布图,这些图件是进行月球地质填图的基础。校正数据反演的FeO和TiO_2分布与前人对Clementine UVVIS数据的反演结果相近,表明干涉成像光谱仪数据具有较大的应用潜力。高地的低铁岩石成分(一般小于8%)佐证了月球月壳形成的过程中的岩浆洋分异假说,而月海玄武岩的TiO_2成分变化范围较大(0~13%)则表明月海玄武岩来源于不同的月幔源区。根据嫦娥一号干涉成像光谱仪全月FeO分布图,可将月球表面物质类型总体划分为高地斜长岩和月海玄武岩,而根据TiO_2分布可以进一步将月海玄武岩划分为5种不同钛含量的玄武岩岩石类型。FeO和TiO_2在全月范围内的分布表明Apollo和Luna返回的月球样品不能够代表全月范围内的矿物成分多样性,月球岩浆演化历史比前人认为的要复杂。未来月球样品返回任务(如嫦娥五号)如能赴这些特殊地区进行取样,将很有可能返回重要的月球科学研究发现和成果。