Kainsaz(CO3)陨石中两个富Al球粒的氧同位素组成特征与形成演化

富Al球粒是原始球粒陨石中一种矿物岩石学特征介于富钙铝包体(CAIs)和镁铁质硅酸盐球粒之间的特殊集合体,所以常常认为富Al球粒在认识CAIs和镁铁质硅酸盐球粒形成演化过程中的相互联系具有特殊意义。然而,对富Al球粒的初始物质组成以及形成演化过程一直存在较多争议,而氧同位素组成研究能够对球粒演化和早期星云环境等提供重要的信息。在本文中我们报导了来自Kainsaz(1937年降落于俄罗斯,CO3型)碳质球粒陨石中的2个富Al球粒(编号K1-CH1和K2-CH2)的矿物岩石学和氧同位素组成特征。K1-CH1的矿物组成主要为橄榄石、低钙辉石和富钙长石,K2-CH2为橄榄石和富钙长石。2个球粒中的矿物均具有贫~(16)O同位素组成特征。K1-CH1中矿物的△~(17)O组成基本上位于2个区间:-11.1‰～-8.7‰和-3.9‰～0.4‰;而K2-CH2的△~(17)O介于-6.6‰～-0.6‰之间,且具有从中部至边部升高的趋势。矿物岩石学和氧同位素特征表明,这2个富Al球粒的初始物质组成为富CAIs和镁铁质硅酸盐。在球粒熔融结晶过程中,与贫~(16)O同位素组成(△~(17)O:-8.7‰～-7.8‰)的星云发生了氧同位素交换。球粒形成后,发生迁移进入陨石母体,在相对更贫~(16)O同位素组成(△~(17)O:-0.6‰～0.4‰)的母体中(流体参与)发生变质作用,并再次发生了氧同位素交换。     

不同类型球粒陨石钙同位素组成特征及对比研究

准确限定球粒陨石的Ca同位素组成对于研究太阳星云物质演化和行星形成都具有重要意义。选取7块典型的球粒陨石,包括3块CV3型陨石(Leoville、Allende和Vigarano)、1块CM2型陨石(Murchison)、1块CO3.2型陨石(Kainsaz)、1块EH4型陨石(Indarch)以及1块H4型陨石(LaPaz Icefield 03601),进行了Ca同位素组成的研究。其中, Kainsaz、Leoville和LaPaz Icefield 03601共3块陨石的Ca同位素组成是首次报道。结果显示:(1)在增大样品量以规避"样品量效应"的情况下,我们对CV群球粒陨石Ca同位素组成进行更加精确的制约,δ^44/40Ca的平均值为0.45‰±0.04‰(n=3, 2SE);(2)碳质球粒陨石的Ca同位素组成相对于硅酸盐地球偏轻,从CV群(0.45‰±0.04‰, 2SE)、CM群(0.73‰±0.04‰, 2SE)到CO群(0.78‰±0.03‰, 2SE)逐渐变重,可能与不同化学群陨石中富钙铝难熔包体(CAIs)丰度的变化有关;(3)顽火辉石球粒陨石和普...     

球粒陨石中富Ca、Al包体成因研究进展与演化模式

富Ca、Al包体(简称CAI)形成于太阳星云演化的最初始阶段,其成因模式主要包括:气—固凝聚、熔融结晶和部分熔融以及高温蒸发作用等。最近,通过对不同球粒陨石化学群中的CAI进行岩石学特征对比研究,发现不同化学群中的CAI具有相似的大小和类型分布特征,表明不同球粒陨石化学群中的CAI极可能具有相似的起源。该结果,与前人的氧同位素、Al—Mg同位素体系以及稀土元素等研究得到的结论一致。不同球粒陨石化学群中的CAI具有相似的成因,并很可能形成于太阳星云的相同区域,随后迁移到不同球粒陨石群的吸积区域。     

陨石氧同位素组成及其地学意义

介绍了各类陨石氧同位素组成的特点,对陨石氧同位素组成的主要成因观点进行了评述,结合地球的原始物质组成,讨论了陨石氧同位素组成的地球科学意义。     

我国某些球粒陨石物质组成的初步研究

据统计,我国现已收集27次石陨石及24次铁陨石(图1)。如图1所示我国陨石的分布与人口密度出现正比关系。石陨石多为普通球粒陨石,其中最大的为吉林陨石雨,共收集到约2500公斤样品。铁陨石中最大的是新疆铁陨石,重约30吨,按其重量居世界第三位。 本文的主要目的是根据已发表的部分资料和笔者的室内工作,对我国部分球粒陨石的物质成分、化学-岩石类型及其形成和演化历史进行初步探讨。     

吉林伊通幔源包体的氧同位素组成

吉林伊通幔源包体的氧同位素组成徐义刚，Ｍ．Ａ．ＭｅｎｚｉｅｓＤ．Ｐ．Ｍａｔｔｅｙ林传勇（中国科学院广州地球化学研究所，广州５１０６４０）（ＤｅｐａｒｔｍｅｎｔｏｆＧｅｏｌｏｇｙ，ＲｏｙａｌＨｏｌｌｏｗａｙＵｎｉｖｅｒｓｉｔｙｏｆＬｏｎｄｏｎ，Ｅｇｈａ...     

中国南极球粒陨石的高精度钾同位素研究

钾和其他中等挥发性元素亏损是类地行星普遍的全岩化学成分特征之一,能用来示踪不同的亏损过程.球粒陨石是组成行星的前体物质,研究球粒陨石中钾同位素的亏损和分异机制,对于太阳系物质或行星的起源、形成和演化具有十分重要的意义.本文利用近年来发展的高精度钾同位素分析技术,测试了 14 个中国南极陨石以及6 个目击型陨石(Murc...     

宁强陨石中不透明矿物集合体的氧同位素和成因研究

宁强碳质球粒陨石的球粒和基质中出现大量圆形的不透明矿物集合体。其中的主要矿物为磁铁矿、富镍金属和硫化物，另有少量磷酸盐、硅酸盐及微量的铂族金属。离子探针测定显示：①磁铁矿的氧同位素组成服从质量分馏[斜率为0.51±0.04,Δ17O为（-2.8±0.4)‰],δ18O值在-15.3‰~-1.6‰的较大范围内变化；②球粒中的橄榄石(Δ17O为-5.0‰）与不透明矿物集合体处于氧同位素不平衡状态。不透明矿物集合体是由小行星母体中的蚀变反应产生的，金属铁被氧化为磁铁矿，同时使剩余的金属富集镍。     

富钙长石-橄榄石包体与其他部分典型包体W-L边的成因

球粒陨石中的富Ca、Al包体(简称CAI)形成于星云演化的最初始阶段,保存了大量星云形成和演化的各种信息。研究认为,包体的成因主要包括星云直接凝聚和熔融结晶,少部分甚至经历过高温蒸发过程。部分CAI最外层具有由一种或几种矿物组成的Warking-Lovering边(简称为W-L边),CAI和其W-L边对于认识早期星云环境和界定CAI的形成时间等均具有重要意义。目前,对于W-L边的形成过程研究并不深入,且一直存在争议。本文主要介绍了三个典型包体:C#1(富钙长石-橄榄石包体)、GRV 022459-2RI5(A型包体)和GRV 021579-3RI5(富尖晶石球粒状包体)及其W-L边的矿物岩石学和氧同位素组成特征。C#1包体明显经历过熔融结晶过程,W-L边氧同位素组成具有与包体内部矿物相似的富~(16)O同位素特征,表明W-L边的成因与包体的形成过程密切相关,形成于同一富~(16)O同位素组成区域,且W-L边属于包体熔融结晶过程后期的产物。矿物岩石学特征表明,GRV 022459-2RI5属于星云直接凝聚形成,其W-L边为包体形成过程最晚期星云凝聚产物。GRV021579-3RI5经历过熔融结晶过程,其W-L边为包体结晶最后阶段的产物。     

Siderophile elements in chondrules of CV chondrites

New bulk compositional data for 34 Allende chondrules are presented. Whole chondrules were analyzed by instrumental neutron activation analysis (INAA). The new data set is evaluated together with older INAA data on Allende chondrules and recent INAA data on Mokoia chondrules. The Ni/Co ratios of 200 chondrules are close to the CI- or solar ratio. The chondritic Ni/Co ratios require an unfractionated chondritic metal source and set a limit to the fraction of metal lost from molten chondrules. The bulk chondrule Fe/Ni and Fe/Co ratios are more variable but on average chondritic. Iridium and other refractory metals have extremely variable concentrations in chondrules. High Ir chondrules have chondritic Ir/Sc ratios. They are dominated by CAI (Ca,Al-rich inclusion) components. Low Ir chondrules have approximately chondritic Ir/Ni ratios reflecting mixing with chondritic metal. In low Ir chondrules Ir correlates and in high Ir chondrules Ir does not correlate with Ni or Co. A large fraction of Ir may have entered chondrules in variable amounts as tiny grains of refractory metal alloys.Most Allende chondrules have Ir/Sc ratios below bulk meteorite ratios. Matrix must have a complementary high Ir/Sc ratio, as bulk Allende has approximately chondritic Ir/Sc ratio. Similarly, the high average Ir/Ni ratios of Allende chondrules must be balanced by low Ir/Ni ratios in matrix to obtain the bulk Allende Ir/Ni ratio, which is close to the average solar system ratio.More recent data on single chondrules from Allende by ICP-MS (Inductively Coupled Plasma Mass Spectrometry) and ICP-OES (Inductively Coupled Optical Emission Spectrometry) show the same trends as the INAA data discussed here.     

Petrology and oxygen isotope compositions of chondrules in E3 chondrites

Chondrules in E3 chondrites differ from those in other chondrite groups. Many contain near-pure endmember enstatite (Fs_<1). Some contain Si-bearing FeNi metal, Cr-bearing troilite, and, in some cases Mg, Mn- and Ca-sulfides. Olivine and more FeO-rich pyroxene grains are present but much less common than in ordinary or carbonaceous chondrite chondrules. In some cases, the FeO-rich grains contain dusty inclusions of metal. The oxygen three-isotope ratios (δ¹⁸O, δ¹⁷O) of olivine and pyroxene in chondrules from E3 chondrites, which are measured using a multi-collection SIMS, show a wide range of values. Most enstatite data plots on the terrestrial fractionation (TF) line near whole rock values and some plot near the ordinary chondrite region on the 3-isotope diagram. Pyroxene with higher FeO contents (∼2-10 wt.% FeO) generally plots on the TF line similar to enstatite, suggesting it formed locally in the EC (enstatite chondrite) region and that oxidation/reduction conditions varied within the E3 chondrite chondrule-forming region. Olivine shows a wide range of correlated δ¹⁸O and δ¹⁷O values and data from two olivine-bearing chondrules form a slope ∼1 mixing line, which is approximately parallel to but distinct from the CCAM (carbonaceous chondrite anhydrous mixing) line. We refer to this as the ECM (enstatite chondrite mixing) line but it also may coincide with a line defined by chondrules from Acfer 094 referred to as the PCM (Primitive Chondrite Mineral) line (Ushikubo et al., 2011). The range of O isotope compositions and mixing behavior in E3 chondrules is similar to that in O and C chondrite groups, indicating similar chondrule-forming processes, solid-gas mixing and possibly similar ¹⁶O-rich precursors solids. However, E3 chondrules formed in a distinct oxygen reservoir.Internal oxygen isotope heterogeneity was found among minerals from some of the chondrules in E3 chondrites suggesting incomplete melting of the chondrules, survival of minerals from previous generations of chondrules, and chondrule recycling. Olivine, possibly a relict grain, in one chondrule has an R chondrite-like oxygen isotope composition and may indicate limited mixing of materials from other reservoirs. Calcium-aluminum-rich inclusions (CAIs) in E3 chondrites have petrologic characteristics and oxygen isotope ratios similar to those in other chondrite groups. However, chondrules from E3 chondrites differ markedly from those in other chondrite groups. From this we conclude that chondrule formation was a local event but CAIs may have all formed in one distinct place and time and were later redistributed to the various chondrule-forming and parent body accretion regions. This also implies that transport mechanisms were less active at the time of and following chondrule formation.     

Mineralogy,petrography, and oxygen and aluminum-magnesium isotope systematics of grossite-bearing refractory inclusions

Grossite (CaAl₄O₇) is one of the one of the first minerals predicted to condense from a gas of solar composition, and therefore could have recorded isotopic compositions of reservoirs during the earliest stages of the Solar System evolution. Grossite-bearing Ca,Al-rich inclusions (CAIs) are a relatively rare type of refractory inclusions in most carbonaceous chondrite groups, except CHs, where they are dominant. We report new and summarize the existing data on the mineralogy, petrography, oxygen and aluminum-magnesium isotope systematics of grossite-bearing CAIs from the CR, CH, CB, CM, CO, and CV carbonaceous chondrites. Grossite-bearing CAIs from unmetamorphosed (petrologic type 2―3.0) carbonaceous chondrites preserved evidence for heterogeneous distribution of ²⁶Al in the protoplanetary disk. The inferred initial ²⁶Al/²⁷Al ratio [(²⁶Al/²⁷Al)₀] in grossite-bearing CAIs is generally bimodal, ˜0 and ˜5×10⁻⁵; the intermediate values are rare. CH and CB chondrites are the only groups where vast majority of grossite-bearing CAIs lacks resolvable excess of radiogenic ²⁶Mg. Grossite-bearing CAIs with approximately the canonical (²⁶Al/²⁷Al)₀ of ˜5×10⁻⁵ are dominant in other chondrite groups. Most grossite-bearing CAIs in type 2–3.0 carbonaceous chondrites have uniform solar-like O-isotope compositions (Δ¹⁷O ˜ ‒24±2‰). Grossite-bearing CAIs surrounded by Wark-Lovering rims in CH chondrites are also isotopically uniform, but show a large range of Δ¹⁷O, from ˜ ‒40‰ to ˜ ‒5‰, suggesting an early generation of gaseous reservoirs with different oxygen-isotope compositions in the protoplanetary disk. Igneous grossite-bearing CAIs surrounded by igneous rims of ±melilite, Al-diopside, and Ca-rich forsterite, found only in CB and CH chondrites, have uniform ¹⁶O-depleted compositions (Δ¹⁷O ˜ ‒14‰ to ‒5‰). These CAIs appear to have experienced complete melting and incomplete O-isotope exchange with a ¹⁶O-poor (Δ¹⁷O ˜ ‒2‰) gas in the CB impact plume generated about 5 Ma after CV CAIs. Grossite-bearing CAIs in metamorphosed (petrologic type >3.0) CO and CV chondrites have heterogeneous Δ¹⁷O resulted from mineralogically-controlled isotope exchange with a ¹⁶O-poor (Δ¹⁷O ˜ ‒2 to 0‰) aqueous fluid on the CO and CV parent asteroids 3–5 Ma after CV CAIs. This exchange affected grossite, krotite, melilite, and perovskite; corundum, hibonite, spinel, diopside, forsterite, and enstatite preserved their initial O-isotope compositions. The internal ²⁶Al-²⁶Mg isochrons in grossite-bearing CAIs from weakly-metamorphosed CO and CV chondrites were not disturbed during this oxygen-isotope exchange.HCCJr is grateful to Klaus Keil for all his sound profession counsel and collegial friendship over the years. He has always been willing to talk and has the generous nature of listening and sharing his thoughts freely and constructively. Professor Klaus Keil has been a mentor to and played a key role in the careers of three of the authors of this paper (ANK, KN, and GRH). He has also influenced the careers of the other authors and most of the people who have worked on meteorites over the past 50+ years. We therefore dedicate this paper to Professor Keil and present it in this Special Issue of Geochemistry.     

Mineralogy and petrology of Al-rich objects and amoeboid olivine aggregates in the CH carbonaceous chondrite North West Africa 739

The aluminum-rich (>10 wt% Al₂O₃) objects in the CH carbonaceous chondrite North West Africa (NWA) 739 include Ca,Al-rich inclusions (CAIs), Al-rich chondrules, and isolated mineral grains (spinel, plagioclase, glass). Based on the major mineralogy, 54 refractory inclusions found in about 1 cm² polished section of NWA 739 can be divided into hibonite-rich (16%), grossite-rich (26%), melilite-rich (28%), spinel-pyroxene-rich (16%) CAIs, and amoeboid olivine aggregates, (AOA's, 17%). Most CAIs are rounded, 25–185 μm (average=70 μm) in apparent diameter, contain abundant, tiny perovskite grains, and typically surrounded by a single- or double-layered rim composed of melilite and/or Al-diopside; occasionally, layers of spinel+hibonite and forsterite are observed. The AOAs are irregularly shaped, 100–250 μm (average=175 μm) in size, and consist of forsterite, Fe,Ni-metal, and CAIs composed of Al-diopside, anorthite, and minor spinel. One AOA contains compact, rounded melilite-spinel-perovskite CAIs and low-Ca pyroxene replacing forsterite. The Al-rich (>10 wt% bulk Al₂O₃) chondrules are divided into Al-diopside-rich and plagioclase-rich. The Al-diopside-rich chondrules, 50–310 μm (average=165 μm) in apparent diameter, consist of Al-diopside, skeletal forsterite, spinel, ±Al-rich low-Ca pyroxene, and ±mesostasis. The plagioclase-rich chondrules, 120–455 μm (average=285 μm) in apparent diameter, are composed of low-Ca and high-Ca pyroxenes, forsterite, anorthitic plagioclase, Fe,Ni-metal nodules, and mesostasis. The isolated spinel occurs as coarse, 50–125 μm in size, subhedral grains, which are probably the fragments of Al-diopside chondrules. The isolated plagioclase grains are too coarse (60–120 μm) to have been produced by disintegration of chondrules or CAIs; they range in composition from nearly pure anorthite to nearly pure albite; their origin is unclear. The Al-rich objects show no evidence for Fe-alkali metasomatic or aqueous alteration; the only exception is an Al-rich chondrule fragment with anorthite replaced by nepheline. They are texturally and mineralogically similar to those in other CH chondrites studied (Acfer 182, ALH85085, PAT91467, NWA 770), but are distinct from the Al-rich objects in other chondrite groups (CM, CO, CR, CV). The CH CAIs are dominated by very refractory minerals, such as hibonite, grossite, perovskite and gehlenitic melilite, and appear to have experienced very low degrees of high-temperature alteration reactions. These include replacement of grossite by melilite, of melilite by anorthite, diopside, and spinel, and of forsterite by low-Ca pyroxene. Only a few CAIs show evidence for melting and multilayered Wark-Lovering rims. These observations may suggest that CH CAIs experienced rather simple formation history and escaped extensive recycling. In order to preserve the high-temperature mineral assemblages, they must have been efficiently isolated from the hot nebular region, like some chondrules and the zoned Fe,Ni-metal grains in CH chondrites.     

徐州地区下古生界碳酸盐岩的碳、氧同位素研究

在已有的对徐州地区下古生界碳酸盐岩详细岩石学研究基础上，系统测试了碳酸盐岩方解石和白云石的碳、氧同位素组成特征；地球化学和岩石学研究相结合，综合提取了碳酸盐岩碳、氧同位素组成的沉积、成岩地质信息；初步探讨了同位素组成的地层变化及其意义。研究结果表明：碳酸盐岩碳同位素组成特征可以指示沉积环境及其演化，开阔陆表海、灰质障壁砂坝、局限陆表海、潮下带、潮渠、藻坪诸沉积相间碳酸盐岩的δ^13C值表现出规律性变化，碳同位素组成变化曲线上的显著正偏移与海侵有关；碳酸盐岩氧同位素组成对成岩环境及其演化有明显响应，淡水成岩环境、潮上成岩环境、潮间成岩环境、潮下成岩环境和埋藏成岩环境具有不同的碳酸盐岩氧同位素组成特征；徐州地区大北望寒武系剖面地层界线附近都有碳、氧同位素组成变化的特征显示，研究工作证实了徐州地区下古生界同位素地层划分的可行性。     

中国大陆科学钻探工程主孔734～933m岩芯矿物的氧同位素和羟基含量研究

中国大陆科学钻探工程(CCSD)主孔位于苏鲁超高压变质带南部的东海县毛北村。本文主要研究深度分别为734.21m～737.16m(Ⅰ)和929.67m～932.86m(Ⅱ)两段榴辉岩与片麻岩互层的主孔岩芯，利用激光氟化法和Fourier变换红外光谱技术分别进行矿物的氧同位素组成和结构羟基含量分析。氧同位素分析表明，两段岩芯的榴辉岩中石榴石的δ^18O分别为 1.0‰～ 3.8‰和-4.1‰～-3、3‰，两段岩芯的片麻岩中石榴石的δ^18O均低达-4‰。表明片麻岩和榴辉岩的原岩均在经历超高压变质作用之前一同遭受过古大气降水的高温热液蚀变作用。在第1段岩芯的榴辉岩和片麻岩接触界线附近发现氧同位素交换前锋，指示板块折返过程中靠近片麻岩的榴辉岩与主要来自片麻岩的退变质流体发生流体-岩石交换，且其退变质程度主要受流体的迁移距离控制。红外光谱分析研究表明，所有石榴石都含有以OH形式存在的结构水，其含量的变化范围很大，为50～776ppm；绿辉石中OH含量范围为321～1636ppm；石英中含有以3596cm^-1为特征峰的结构水，但是含量很少。将剖面氧同位素和结构羟基含量的分析结果相结合，我们发现石榴石和绿辉石等矿物的氧同位素组成随着深度的变化与对应矿物的OH含量具有一定的相关性。这证明板块折返过程中的高压退变质作用及其伴生的局部流体活动可能是造成超高压变质矿物之间氧同位素不平衡的主要原因，并且氧同位素不平衡的程度主要受退变质作用发生时的局部水/岩比控制。因此，在深俯冲板块折返过程中，名义上无水矿物中结构水的出溶可以是退变质流体的重要来源。     

胶东地块西部变质岩锆石U-Pb定年和氧同位素研究

对胶东地块西部变质岩作了系统的锆石U-Pb定年和矿物氧同位素分析,结果对这些变质岩的原岩性质和变质时代提供了制约。研究得到:(2)2个TTG片麻岩的原岩谐和年龄分别为2692±14Ma和2691±12Ma,部分锆石记录了1.7Ga～1.8Ga左右的变质事件。岩浆锆石δ~(18)O值为5.11～5.55‰,指示TTG岩浆在成因上与幔源岩石关系密切;(2)呈透镜状包体分布于TTG片麻岩中的斜长角闪岩全岩δ~(18)O估计值总体在6.0～6.5‰之间,表明斜长角闪岩原岩同样具幔源性质,其原岩初始氧同位素组成总体未受后期变质作用改造,但局部有低δ~(18)O值(3.6‰)斜长角闪岩分布,指示胶东地块西部同样存在δ~(18)O亏损事件;(3)粉子山群长英质副片麻岩具有较高的氧同位素组成,全岩δ~(18)O估计值在12.3～14.5‰之间,锆石δ~(18)O值高达9.92‰,指示其源区物质为高δ~(18)O值表壳岩。粉子山群斜长角闪岩全岩δ~(18)O估计值在5.5‰左右,表明其原岩具有幔源性质,原岩初始氧同位素组成也未受后期变质作用的明显改造;(4)粉子山群混合岩化变质作用时间为1748±22Ma,斜长角闪质混合岩中变质新生锆石δ~(18)O值为6.07‰,长英质混合岩中变质新生锆石δ~(18)O值为6.88～7.67‰,指示在混合岩化变质作用过程中有外部高δ~(18)O值流体加入,引起混合岩氧同位素组成不同程度地升高;(5)粉子山群中橄榄大理岩岩浆核锆石U-Pb不一致线上、下交点年龄分别为769±48Ma和215±34Ma,分别代表岩浆锆石结晶年龄和变质年龄,说明胶东地块西部同样存在新元古代岩浆活动,并遭受到三叠纪变质作用;(6)分布于TTG片麻岩中的基性麻粒岩原岩年龄为2379±54Ma,麻粒岩相变质作用时间为1794±41Ma,与混合岩化变质作用时间基本一致。麻粒岩相变质锆石δ~(18)O值为4.75‰,氧同位素研究表明基性麻粒岩原岩具幔源性质,其原岩氧同位素组成未受到后期变质作用改造。胶东地块西部新元古代岩浆活动、印支期变质时代和~(18)O亏损事件的产出指示,胶东地块西部有可能属于扬子板块,对应于扬子板块北缘新元古代裂谷岩浆侵位时裂谷肩部的北翼古老围岩。在印支期陆壳俯冲过程中,整个胶东地块西部可能并没有俯冲到地幔深度。     

胶东地块东部变质岩锆石U-Pb定年和氧同位素研究

对胶东地块东部高压-超高压变质岩作了系统的锆石U-Ph定年和矿物氧同位素分析,结果对这些变质岩的原岩性质提供了制约。研究得到:(1)区域花岗片麻岩及岩浆锆石普遍不同程度地亏损~(18)O,3个片庥岩样品中岩浆核锆石U-Pb年龄分别为723±36Ma、738±17Ma和744±63Ma,低δ~(18)O值(-0.42～4.14‰)岩浆核锆石说明其原岩为新元古代低δ~(18)O值岩浆岩,石英-石榴石氧同位素温度及少量印支期变质锆石的出现,指示片麻岩与榴辉岩曾经共同经历了印支期超高压变质作用;(2)花岗片麻岩中的榴辉岩原岩年龄有两种,一种是新元古代,其U-Ph年龄为806±79Ma。另一种是古元古代晚期,其 U-Pb年龄为1838±41Ma。这2个榴辉岩的超高压变质年龄分别为229±3Ma和242±21Ma。多数榴辉岩中的变质增生或变质重结晶锆石也具有低δ~(18)O值特征(0.22～3.4‰),指示在榴辉宕相变质作用之前,这些榴辉岩原岩为低δ~(18)O值蚀变岩或低δ~(18)O值基性岩浆岩;(3)大理岩中榴辉岩变质增生锆石δ~(18)O值高达15.9‰,U-Pb年龄为229±4Ma,指示在榴辉岩相变质作用之前,榴辉岩原岩与大理岩一样具有高δ~(18)O值;(4)斜长角闪岩的原岩U-Pb年龄为1719±18Ma,与同时期榴辉岩原岩一起构成扬子板块北缘新元古代岩浆侵位时的裂谷肩部围岩,在三叠纪大陆碰撞时同样受到变质改造。     

Evaluation of oxygen isotopes in carbonate as an indicator of lake evolution in arid areas: The modern Qinghai Lake, Qinghai–Tibet Plateau

The oxygen isotopic composition of carbonate in lakes has been used as a useful indicator in Palaeolimnological research, and has made some important contributions to our understanding of lacustrine systems. For modern lakes in arid or cold areas, however, there are few data available to test the effect of lake salinity and temperature on the oxygen isotopic composition of various carbonate sources such as ostracod, bulk carbonate, and fine-grained carbonate (< 60 μm). Here we examined the oxygen isotopic composition of ostracods, bulk carbonate, and fine-grained carbonates, as well as that of coexisting water from Lake Qinghai and the smaller surrounding lakes and ponds on the Qinghai–Tibet Plateau. Our investigation highlights three key effects. First, the oxygen isotopic composition of ostracods, bulk carbonate, and fine-grained carbonate in the lakes and ponds shows a clear response to lake water δ¹⁸O values, and these vary with water salinity. The relationship between lake water δ¹⁸O and salinity is not only dominated by the evaporation/freshwater input ratios, but is also controlled by the distance to the mouth of the major rivers supplying to the lake. Second, the ostracod, bulk carbonate, and fine-grained carbonate show similar isotopic change trends in the study area, and oxygen isotopic differences between ostracods and authigenic carbonate may be explained by the different water temperatures and very small ‘vital offsets’ of ostracods. Finally, the effect of water depth on temperature leads to increasing δ¹⁸O values in carbonates as water depth increases, both in benthic ostracods living on the lake bottom, as well as in bulk carbonate precipitated at the water surface.For arid, high-altitude Lake Qinghai, our results suggest that variations in the δ¹⁸O values of carbonate in Lake Qinghai are mainly controlled by the oxygen-isotope ratio of the lake water changing with water salinity. As a secondary effect, increasing water depth leads to cooler bottom and surface water, which may result in more positive δ¹⁸O values of ostracod and bulk carbonate.