上地幔Os同位素组成的演化

Re-Os同位素体系为研究地幔的成分-结构-演化提供了新的地球化学示踪和定年的工具.上地幔Os同位素组成演化的球粒陨石模型是Re-Os体系用于地幔物质定年的基础, 尤其在采用Re亏损模式年龄和Os同位素代理等时线年龄时.综合了铁陨石和各类球粒陨石、地幔橄榄岩包体和蛇绿岩豆荚状铬铁矿的Re-Os同位素体系研究的近期成果, 为认识对流上地幔Os同位素组成的演化提供了制约.对河北遵化蛇绿岩豆荚状铬铁矿岩的研究, 获得新太古代(2.5 Ga)时形成豆荚状铬铁矿的对流上地幔的187Os/188Os=0.110 2, 与球粒陨石型模式的一致.文献中常用的球粒陨石模式的参数如下: 地球形成时(4.558 Ga)初始值187Os/186Os为0.095 31, 现代值分别采用碳质球粒陨石的187Os/186Os比值为0.127 0和原始上地幔(PUM)的187Os/186Os比值为0.129 6, PUM与普通球粒陨石和顽火球粒陨石的187Os/186Os比值接近.      

浙江长兴“金钉子”灰岩Re Os富集机制研究

通过对浙江长兴煤山D剖面二叠—三叠"金钉子"灰岩样品Re-Os同位素、主微量元素和有机碳测定,对不同层位灰岩的沉积环境进行了判别。通过分析灰岩主微量元素、有机碳与Re、Os含量的相关性,探索性地研究了灰岩中Re、Os富集机制。研究发现,灰岩中Re、Os的富集主要受氧化还原作用影响,Re只有在还原环境下,才会被灰岩中的有机物富集,此时灰岩中Re含量较高,适用于Re-Os同位素定年,而Re在氧化环境下很难被灰岩中有机质富集。Os在还原环境下同样被有机质富集,但氧化环境下,部分Os也可以被灰岩地层中含铁、铜等自生矿物吸附富集,含铁、铜等自生矿物Os同位素比值可以代表沉积时海水Os同位素特征。Re、Os在灰岩中的富集机制研究对于将Re-Os同位素应用于灰岩地层精确定年及古环境示踪具有重要意义。Re、Os在不同氧化还原条件下的富集差异导致了还原环境沉积的灰岩中187 Re/188 Os要大于氧化环境灰岩中187 Re/188 Os,灰岩中187 Re/188 Os变化对研究古海洋沉积氧化还原环境可能具有一定指示意义。     

月球物质的Re-Os同位素组成研究：对月球后期增生历史的指示

Re-Os同位素体系是理解月球强亲铁元素的分布规律和示踪月球的后期增生历史的重要手段。目前人们对月球物质Re-Os同位素成分的了解还是十分有限的,已有的Re-Os同位素数据显示一些能代表月幔成分特征的月海玄武岩具有很低的Re和Os的浓度,以及类似于球粒陨石的187Os／188Os成分特征,而月球火山玻璃和月壤等表现出相对高的Re-Os丰度和相对富放射成因Re-Os同位素成分。一般认为月球月幔的Re、0s和其他强亲铁元素相对球粒陨石是非常亏损的,而地球地幔则具有相对较高的强亲铁元素丰度（0．008倍CI球粒陨石的丰度）。新的Re-Os同位素结果证明月幔确实是亏损的,但是月球和地球在太阳系演化的较晚时期都有外来的球粒陨石物质的大量加入,即后期增生（late accretion）过程,导致了月球和地球上部物质（如月球火山玻璃、月壤等）相对地富集Os同位素和强亲铁元素,这些外来物质的后期增生可能是长期和持续的,增生过程主要发生在3．9～4．4Ga。但目前仍不清楚后期增生的陨石物质是被逐渐加入的,还是在一个相对较短的时期大量加入的,因此尚需对更多的月球物质做进一步的Re-Os同位素和强亲铁元素成分的研究。     

Re-Os同位素测年法在油气成藏年代学的研究进展

铼—锇(Re-Os)同位素应用于油气成藏年代学是近10年来的一个前沿领域,在国际上已取得了重要成果,目前国内对此方法的应用还较缺乏。利用Re-Os同位素测年法开展页岩或沥青等富有机质沉积岩的研究,可以精确厘定油气运移和充注时间,也可以有效示踪烃源岩。在阅读国内外大量文献的基础上,概述了Re-Os同位素定年原理,分析了海水—沉积物中Re和Os元素的富集过程,总结了Re-Os同位素测年的测试对象、样品准备和分析测试方法。指出初始187Os/188Os比值不仅可以限定油气生成和油气充注的年龄,还可以有效评价源—油关系;放射成因的187Os/188Os比值与烃源岩年龄呈正相关。认为烃类成熟度、生物降解作用和水洗作用不足以造成Re-Os等时线图中出现离散点,而初始187Os/188Os比值变化、沉积后Re和Os的流动性和硫酸盐热化学还原作用是引起Re-Os等时线图中出现离散点的3个主要原因。Re-Os年龄的重现性和准确性与样品颗粒的大小及取样量密切相关。相对于其他同位素测年法,Re-Os同位素测年法的最大优势在于对直接参与油气成藏的地质体进行研究,可以得到油气成藏期的直接证据。最后探讨了现阶段ReOs同位素体系研究中尚存在的问题,就未来研究热点和发展方向做出展望,以期能有效推动Re-Os同位素定年相关的理论和技术的深入发展。     

利用多接收器电感耦合等离子体质谱仪(MC-ICPMS)测定镁铁-超镁铁质岩石中的铼-锇同位素组成

报道了用多接收器电感耦合等离子体质谱仪(MC-ICPMS)测定Re-Os同位素组成的质谱方法和化学分离方法,并应用该方法测定了天然镁铁-超镁铁质岩石样品中的Os同位素组成及Re、Os含量.Re同位素组成的MC-ICPMS测定利用膜除溶雾化器(Aridus)和静态法拉第杯接收的方式完成,采用Ir标准溶液在线校正仪器的质量分馏.Os同位素组成的MC-ICPMS测定采用常规雾化器和离子计数器静态接收的方式完成,并用10%的HCl-EtOH和10%的HCl溶液交替清洗进样系统来消除Os的"记忆效应".岩石样品的Re和Os化学分离采用Carius管溶样法,结合CCl4萃取以及微蒸馏的方法分离纯化Os,利用阴离子交换树脂的方法分离纯化Re.运用上述方法,对6个镁铁-超镁铁质岩石样品中的Re、Os含量和187Os/188Os同位素比值进行了测定,获得了理想的分析结果.     

油气成藏定年的Re-Os同位素方法应用研究

Re和Os易于被有机物捕获而富集,并长期稳定地保存在烃源岩、原油和沥青中而保持良好的封闭体系.可以对烃源岩、原油和沥青进行Re-Os同位素直接定年,获得与油气成藏相关的精确的绝对年龄信息.Re-Os同位素实验分析包括样品的溶解、Re和Os的化学分离与纯化、Re和Os同位素的质谱测定.原油中沥青质组分的Re,Os同位素组成能够近似代表全油的Re,Os同位素组成,对原油进行Re-Os同位素分析实质就是对原油中的沥青质组分中的Re-Os同位素体系进行分析,其年龄记录的是油气生成的年龄,原油和烃源岩的187Os/188 Os比值的对比可以进行油源示踪.沥青Re-Os同位素等时线年龄揭示的是油气大量生成运移的时间,年龄数据分散的主要原因是具有不同187 Os/188 Os初始比值的烃源岩对Re-Os体系的贡献.川西龙门山北段矿山梁下寒武统沥青Re-Os同位素组成和等时线年龄指示了油气生成和运移的时间发生在～164 Ma,并来源于两种烃源岩.Re-Os同位素体系的封闭性、等时线年龄的精度和油气地质意义、烃源岩多期熟化作用和混源作用的影响等方面还值得进一步深入研究.Re-Os同位素方法将在油气成藏年代学领域,特别是在碳酸盐岩地区的油气成藏定年方面具有广泛的应用前景.     

Re-Os同位素体系在金属矿床中的应用

Re-Os同位素体系已成为金属矿床定年和示踪的重要手段之一。文章在简述Re-Os同位素体系基本原理基础上,综述了国内外的最新研究成果,认为Re-Os同位素测试对象不再局限于辉钼矿和铜镍硫化物矿石,黄铁矿、毒砂、磁黄铁矿、镍黄铁矿、闪锌矿等也常作为测试对象用于金矿床、铅锌矿床、沉积喷流型钴(金)等矿床的定年。地壳岩石与原始地幔相比,具有较高的187 Os/188 Os比值、γOs值以及Re/Os比值,因此,硫化物或矿石的Re-Os同位素组成和普通Os—Re/Os比值图解可以揭示斑岩矿床、金矿、铅锌矿以及铜镍硫化物矿的成矿物质来源。辉钼矿则可以通过Re含量来示踪成矿物质来源。Re-Os同位素也可与其他同位素结合(如187 Os/188 Os-87Sr/86Sr)共同判明不同端元组分对成矿的贡献。     

含辉钼矿全岩样品Re-Os同位素定年研究:在北京大庄科钼矿床中的应用

采用硝酸在比色管中对辉钼矿样品中Re含量进行初测的方法,测得辉钼矿标准样品JDC Re含量与推荐值在误差范围内基本一致,与传统的Carius管法相比,该方法具有简便快速的特点。传统的辉钼矿Re-Os同位素定年分析对象为辉钼矿单矿物,根据所测得的187Re/187Os值获得辉钼矿的Re-Os年龄,Re、Os在辉钼矿中大量富集,而在硅酸盐矿物中几乎没有,探索性地对含有辉钼矿的全岩样品进行Re-Os同位素定年,虽然所得Re、Os含量偏低,但187Re/187Os值不会变。该方法省去了选样过程花费的大量时间,避免了选样过程中可能造成的交叉污染。采用同位素稀释Carius管逆王水法探索性地对北京大庄科钼矿床中含辉钼矿全岩样品进行Re-Os同位素年龄测定,获得了(137.6±3.7)Ma精确的等时线年龄,与挑选出辉钼矿单矿物样品的Re-Os同位素等时线年龄(136.8±2.6)Ma吻合较好,直接厘定了大庄科钼矿的成矿时代。该年龄与矿区汉家川石英二长岩锆石U-Pb年龄一致,表明大庄科钼矿的形成与汉家川石英二长岩关系较为密切,为中国东部第二期大规模成矿作用的产物,形成于中国东部岩石圈伸展环境。     

一种高纯度锇盐中锇含量的重量法测定

<正>Re-Os体系是一种重要的放射性同位素体系,187Re通过β衰变成187Os,因此可以利用Re-Os体系定年,它是目前厘定金属矿床成矿时代的最直接手段。Re和Os都是高亲铁性元素,集中分布在地核内,地幔及地壳丰度极低,对于常见地质样品,要想获得准确的Re、Os含量必须使用同位素稀释法进行测定。同位素稀释法是一种高精度的化学分析方法,向样品中加入已知质量和同位素组成的稀释剂,待样品溶解、同位素交换平衡后,测定样品+稀释剂的同位素组成变化,以此计算样品中待测     

关于《新疆喀拉通克铜镍硫化物矿床Re-Os同位素测年及成矿物质来源示踪》一文中γOs值计算错误的更正

笔者发表于本刊2005年第4期上《新疆喀拉通克铜镍硫化物矿床Re_Os同位素测年及成矿物质来源示踪》一文由于在计算γOs值时,误将(187Os/188Os)样品以(187Os/188Os)样品(t)代入公式计算,导致判断岩体形成过程中壳幔混染程度时出现错误,作者特刊登此更正声明,希望得到编辑部和学者们的谅解。由公式(187Os/188Os)(t)=(187Os/188Os)-(187Re/188Os)·(eλt-1)计算的样品的(187Os/188Os)(t)结果及利用公式γOs(t)=100·[(187Os/188Os)(t)/(187Os/188Os)球粒陨石(t)-1]重新计算的γOs(t)与原结果一起列于下表。重新计算的γOs值为100.6～12…     

Re-Os and Pd-Ag systematics in Group IIIAB irons and in pallasites

Using improved analytical techniques, which reduce the Re blanks by factors of 8 to 10, we report new Re-Os data on low Re and low PGE pallasites (PAL-anom) and IIIAB irons. The new pallasite samples nearly double the observed range in Re/Os for pallasites and allow the determination of an isochron of slope 0.0775 ± 0.0008 (T = 4.50 ± 0.04 Ga, using the adjusted λ¹⁸⁷Re = 1.66 × 10⁻¹¹ a⁻¹) and initial (¹⁸⁷Os/¹⁸⁸Os)₀ = 0.09599 ± 0.00046. If the data on different groups of pallasites (including the “anomalous” pallasites) are considered to define a whole-rock isochron, their formation would appear to be distinctly younger than for the iron meteorites by ∼60 Ma. Five IIIAB irons (Acuna, Bella Roca, Chupaderos, Grant, and Bear Creek), with Re contents ranging from 0.9 to 2.8 ppb, show limited Re/Os fractionation and plot within errors on the IIAB iron meteorite isochron of slope 0.07848 ± 0.00018 (T = 4.56 ± 0.01 Ga) and initial (¹⁸⁷Os/¹⁸⁸Os)₀ = 0.09563 ± 0.00011. Many of the meteorites were analyzed also for Pd-Ag and show ¹⁰⁷Ag enrichments correlated with Pd/Ag, requiring early formation and fractionation of the FeNi metal, in a narrow time interval, after injection of live ¹⁰⁷Pd (t_1/2 = 6.5 Ma) into the solar nebula. Based on Pd-Ag, the typical range in relative ages of these meteorites is ≤10 Ma. The Pd-Ag results suggest early formation and preservation of the ¹⁰⁷Pd-¹⁰⁷Ag systematics, both for IIIAB irons and for pallasites, while the younger Re-Os apparent age for pallasites suggests that the Re-Os system in pallasites was subject to re-equilibration. The low Re and low PGE pallasites show significant Re/Os fractionation (higher Re/Os) as the Re and PGE contents decrease. By contrast, the IIIAB irons show a restricted range in Re/Os, even for samples with extremely low Re and PGE contents. There is a good correlation of Re and Ir contents. The correlation of Re and Os contents for IIIAB irons shows a similar complex pattern as observed for IIAB irons (Morgan et al., 1995), and neither can be ascribed to a continuous fractional crystallization process with uniform solid-metal/liquid-metal distribution coefficients.     

Comparative Re-Os systematics of chondrites: Implications regarding early solar system processes

A suite of 47 carbonaceous, enstatite, and ordinary chondrites are examined for Re-Os isotopic systematics. There are significant differences in the ¹⁸⁷Re/¹⁸⁸Os and ¹⁸⁷Os/¹⁸⁸Os ratios of carbonaceous chondrites compared with ordinary and enstatite chondrites. The average ¹⁸⁷Re/¹⁸⁸Os for carbonaceous chondrites is 0.392 ± 0.015 (excluding the CK chondrite, Karoonda), compared with 0.422 ± 0.025 and 0.421 ± 0.013 for ordinary and enstatite chondrites (1σ standard deviations). These ratios, recast into elemental Re/Os ratios, are as follows: 0.0814 ± 0.0031, 0.0876 ± 0.0052 and 0.0874 ± 0.0027, respectively. Correspondingly, the ¹⁸⁷Os/¹⁸⁸Os ratios of carbonaceous chondrites average 0.1262 ± 0.0006 (excluding Karoonda), and ordinary and enstatite chondrites average 0.1283 ± 0.0017 and 0.1281 ± 0.0004, respectively (1σ standard deviations). The new results indicate that the Re/Os ratios of meteorites within each group are, in general, quite uniform. The minimal overlap between the isotopic compositions of ordinary and enstatite chondrites vs. carbonaceous chondrites indicates long-term differences in Re/Os for these materials, most likely reflecting chemical fractionation early in solar system history.A majority of the chondrites do not plot within analytical uncertainties of a 4.56-Ga reference isochron. Most of the deviations from the isochron are consistent with minor, relatively recent redistribution of Re and/or Os on a scale of millimeters to centimeters. Some instances of the redistribution may be attributed to terrestrial weathering; others are most likely the result of aqueous alteration or shock events on the parent body within the past 2 Ga.The ¹⁸⁷Os/¹⁸⁸Os ratio of Earth’s primitive upper mantle has been estimated to be 0.1296 ± 8. If this composition was set via addition of a late veneer of planetesimals after core formation, the composition suggests the veneer was dominated by materials that had Re/Os ratios most similar to ordinary and enstatite chondrites.     

Pt-Re-Os systematics of group IIAB and IIIAB iron meteorites

The Pt-Re-Os isotopic and elemental systematics of 13 group IIAB and 23 group IIIAB iron meteorites are examined. As has been noted previously for iron meteorite groups and experimental systems, solid metal-liquid metal bulk distribution coefficients (D values) for both IIAB and IIIAB systems show D_Os>D_Re>>D_Pt>1 during the initial stages of core crystallization. Assuming closed-system crystallization, the latter stages of crystallization for each core are generally characterized by D_Pt>D_Re>D_Os. The processes governing the concentrations of these elements are much more complex in the IIIAB core relative to the IIAB core. Several crystallization models utilizing different starting parameters and bulk distribution coefficients are considered for the Re-Os pair. Each model has flaws, but in general, the results suggest that the concentrations of these elements were dominated by equilibrium crystallization and subsequent interactions between solid metal and both equilibrium and evolved melts. Late additions of primitive metal to either core were likely minor or nonexistent.The ¹⁸⁷Re-¹⁸⁷Os systematics of the IIAB and IIIAB groups are consistent with generally closed-system behavior for both elements since the first several tens of Ma of the formation of the solar system, consistent with short-lived chronometers. The Re-Os isochron ages for the complete suites of IIAB and IIIAB irons are 4530 ± 50 Ma and 4517 ± 32 Ma, respectively, and are similar to previously reported Re-Os ages for the lower-Ni endmembers of these two groups. Both isochrons are consistent with, but do not require crystallization of the entire groups within 10-30 Ma of the initiation of crystallization.The first high-precision ¹⁹⁰Pt-¹⁸⁶Os isochrons for IIAB and IIIAB irons are presented. The Pt-Os isochron ages for the IIAB and IIIAB irons, calculated using the current best estimate of the λ for ¹⁹⁰Pt, are 4323 ± 80 Ma and 4325 ± 26 Ma respectively. The Re-Os and Pt-Os ages do not overlap within the uncertainties. The younger apparent ages recorded by the Pt-Os system likely reflect error in the ¹⁹⁰Pt decay constant. The slope from the Pt-Os isochron is combined with the age from the Re-Os isochron for the IIIAB irons to calculate a revised λ of 1.415 × 10⁻¹² a⁻¹ for ¹⁹⁰Pt, although additional study of this decay constant is still needed.     

班公湖MOR型蛇绿岩Re-Os同位素特征对班公湖-怒江特提斯洋裂解时间的制约

西藏北部班公湖MOR型蛇绿岩主要由角砾状的地幔橄榄岩和玄武岩组成,其中地幔橄榄岩主要是低Cr#尖晶石相含单斜辉石(Cpx)方辉橄榄岩和少量不含Cpx的方辉橄榄岩,玄武岩具有MORB地球化学特点。岩石地球化学特征和二元混合模拟计算表明,含Cpx方辉橄榄岩是由较为亏损的方辉橄榄岩与玄武质熔体发生反应再富集形成的,玄武质熔体和方辉橄榄岩的混合比例为1∶9至1∶4。9个含Cpx方辉橄榄岩样品(含5个重复测试样)的Re和Os含量分别为0.19×10-9~1.49×10-9和2.91×10-9~5.40×10-9,187Re/188Os变化范围为0.169±0.009(2σ)~1.833±0.183(2σ),187Os/188Os变化范围相对较小,介于0.121 13±0.000 44~0.128 53±0.000 36(2σ)之间。含Cpx方辉橄榄岩的Re-Os参考等时线年龄为254±28 Ma。由于不同比例熔体的加入造成橄榄岩具有不同的Re/Os比值,因而不同含Cpx方辉橄榄岩样品具有不同187Os/188Os比值。样品的Re含量与烧失量中的H2O没有相关性,说明蛇纹石化对样品Re-Os体系的影响可以忽略,Re-Os同位素体系在低温地质作用下能够保持相对封闭。参考等时线年龄可能代表亏损方辉橄榄岩与玄武质熔体发生反应的时间,即含Cpx方辉橄榄岩的形成年龄,它表明在该时期特提斯洋经历了一次构造热事件。这一构造岩浆热事件的时间与早期定义的班公湖-怒江特提斯洋的裂解时间晚二叠世至早三叠世较为一致,推测本文MOR型蛇绿岩地幔橄榄岩的Re-Os同位素年龄可能代表班公湖-怒江特提斯洋开始裂解的时间。     

Re-Os同位素体系在蛇绿岩应用研究中的进展

Re-Os不同于由亲石元素构成的同位素体系，在原始上地幔（PUN）部分熔融过程中，母体Re是中等不相容元素，优先进入熔体相，子体Os是强相容元素，富集在残留相中，是研究蛇绿岩的极好示踪剂。在蛇绿岩应用研究中已经取得了4个方面的进展：（1）明确了熔体相的Re／Os和^187Os／^188Os比值高，而残留相的低；（2）铬铁矿中铂族元素矿物（PGM）的Re亏损年龄（TRD）证实了蛇绿岩中复杂的超镁铁岩体是多阶段部分熔融的产物；（3）现代大洋橄榄岩和玄武岩的Re-Os同位素研究表明熔体相和残留相的^187Os／^188Os比值在高于亏损地幔值（DMM）的部分是一致的，而低于DMM的存在不一致性，为研究蛇绿岩中熔体相与残留相是否存在“耦合”关系提供了新的制约因素；（4）揭示了蛇绿岩地幔橄榄岩中含有古大陆岩石圈地幔，这是前所未知的。虽然取得了不少进展，但是由于Re-Os同位素体系用于蛇绿岩研究的时间较短，尚存在一些问题，如显生宙蛇绿岩地幔橄榄岩的定年问题，有待进一步深化研究。     

含有普通锇的辉钼矿Re-Os同位素定年研究

通过大量数据统计,表明较高比例的辉钼矿中存在普通锇。普通锇可能以类质同像形式存在于辉钼矿样品中,理论上辉钼矿中可能含有较高含量普通锇。辉钼矿样品含有较高含量普通锇可能对Re-Os定年结果产生很大影响,从原理上并结合实例证实了普通锇含量对辉钼矿Re-Os年龄影响程度。对于一般辉钼矿样品来讲,如果187Os总量(放射成因187Os与非放射成因187Os之和)与普通锇比值小于20,需要考虑普通锇对Re-Os模式年龄的影响,并提出了对于含有普通锇辉钼矿模式年龄的计算方法。先做出187Os/188Os-187Re/188Os等时线,求得初始187Os/188Os值,再根据初始187Os/188Os值和单个样品的普Os含量求得非放射成因的普Os中187Os的量。最后根据Re含量以及放射成因187Os含量得到模式年龄。     

Assessment of the Re decay constant by cross calibration of Re-Os molybdenite and U-Pb zircon chronometers in magmatic ore systems

The past decade has seen renewed interest in ¹⁸⁷Re-¹⁸⁷Os geochronology using a variety of matrices including sulfide minerals, shales and meteorites. The most widely used value of the ¹⁸⁷Re decay constant (λ¹⁸⁷Re) is 1.666 ± 0.005 × 10⁻¹¹ a⁻¹ (±0.31%), which is based on cross calibration of Re-Os and Pb-Pb chronometers for certain meteorites [Smoliar M. I., Walker R. J., and Morgan J. W. (1996) Re-Os isotope constraints on the age of Group IIA, IIIA, IVA, and IVB iron meteorites. Science271, 1099-1102]. However, other recent studies have yielded alternate values of λ¹⁸⁷Re, based upon either direct counting experiments or analysis of meteorites. Here, we provide an independent assessment of λ¹⁸⁷Re, using methodology, sample materials, and preparation of Os standard solutions different from those of Smoliar et al. (1996). Combining Re-Os age data for molybdenite formed in magmatic ore deposits, with the U-Pb zircon age of the magmatic rocks, a refined λ¹⁸⁷Re value is determined by averaging 11 individual cross-calibration experiments spanning ca. 2700 Ma of Earth history. Using the U decay constants of Jaffey [Jaffey A. H., Flynn K. F., Glendenin L. E., Bentley W. C., and Essling A. M. (1971) Precision measurement of half-lives and specific activities of 235U and 238U. Phys. Rev.4, 1889-1906], a value for λ¹⁸⁷Re of 1.6668 ± 0.0034 × 10⁻¹¹ a⁻¹ is determined. Using the λ²³⁸U value of Jaffey et al. (1971) and λ²³⁵U value of Schoene [Schoene B., Crowley J. L., Condon D. J., Schmitz M. D., and Bowring S. A. (2006) Reassessing the uranium decay constants for geochronology using ID-TIMS U-Pb data. Geochim. Cosmochim. Acta70, 426-445], a value for λ¹⁸⁷Re of 1.6689 ± 0.0031 × 10⁻¹¹ a⁻¹ is determined. These values are nominally higher (ca. 0.1 and ca. 0.2%) than the value determined by Smoliar et al. [Smoliar M. I., Walker R. J., and Morgan J. W. (1996) Re-Os isotope constraints on the age of Group IIA, IIIA, IVA, and IVB iron meteorites. Science271, 1099-1102], but within calculated uncertainty. Further refinement of λ¹⁸⁷Re by cross calibrating the molybdenite and U-Pb zircon chronometers should be possible by utilizing high precision, single-grain, chemical abrasion zircon U-Pb analyses.     

Highly siderophile element evidence for early solar system processes in components from ordinary chondrites

Separated magnetic and nonmagnetic components from the ordinary chondrites Dhajala (H3.8) and Ochansk (H4) were analyzed for their Re-Os isotopic compositions, as well as for the abundances of the highly siderophile elements (HSE) Re, Os, Ir, Ru, Pt and Pd. The Re-Os isotopic systematics of these components are used to constrain the timing of HSE fractionations, and assess the level of open-system behavior of these elements in each of the different components. The high precision, isotope dilution mass spectrometric analyses of the HSE are used to constrain the origins of, and possible relations between some of the diverse components present in these chondrites. The relative and absolute abundances of the HSE differ considerably among the components. Metal fractions have Re/Os that are factors of ∼2 (Dhajala) to ∼3 (Ochansk) higher than those of their nonmagnetic fractions. The isotopic data for both meteorites are consistent with the largest Re-Os fractionations occurring between metal and nonmagnetic components early in solar system history, although minor to moderate late stage, open-system behavior, and limited variations in Re/Os preclude a precise determination of the age for that fractionation. Open-system behavior is generally absent to minor in the metal fractions, and highly variable in nonmagnetic fractions. Re/Os ratios of nonmagnetic fractions deviate as much as 40% from a primordial isochron. Although some deviations are large for isochron applications, nearly all are negligible with respect to consideration of fractionation processes controlling the HSE.Metal from both meteorites contains about 90% of the total budget of HSE. Metal in Ochansk has ∼2 to 10 times the abundances of the bulk meteorite, while metal from the matrix of Dhajala has ∼2 to 4 times the abundances of the bulk. Fine metal in both meteorites has higher abundances than coarse metal, as has been previously observed. Nonmagnetic components, consisting of chondrules and matrix from which metal was removed in the laboratory, have highly fractionated HSE, characterized by much lower Re/Os than the bulk meteorites, as well as large relative depletions in Pd. The abundances of Re, Os, Ir, Ru and Pt in the nonmagnetic fractions are 14-120 ng/g, much higher than would be expected if they had equilibrated with the metal phases present (150-16,000 ng/g). Collectively, the data are consistent with the HSE budget in ordinary chondrites being dominated by two HSE-bearing carrier phases with distinct compositions. These phases formed separately, and never subsequently equilibrated. Metal components incorporated a HSE carrier that formed at high through moderate temperatures and relatively high pressures, such that the relatively volatile Pd behaved coherently with the more refractory HSE. Nonmagnetic fractions from both chondrules and matrix have HSE compositions that likely require at least two processes that fractionated the HSE. Depletions in Pd are consistent with the presence of HSE carriers that formed as either highly refractory condensates, or residues of high degrees of metal melting. Depletions in Re may implicate a period of relatively high f_O2 during which a volatile form of Re was separated from the other HSE.     

Osmium isotope systematics of ureilites

The ¹⁸⁷Os/¹⁸⁸Os for 22 ureilite whole rock samples, including monomict, augite-bearing, and polymict lithologies, were examined in order to constrain the provenance and subsequent magmatic processing of the ureilite parent body (or bodies). The Re/Os ratios of most ureilites show evidence for a recent disturbance, probably related to Re mobility during weathering, and no meaningful chronological information can be extracted from the present data set. The ureilite ¹⁸⁷Os/¹⁸⁸Os ratios span a range from 0.11739 to 0.13018, with an average of 0.1258 ± 0.0023 (1σ), similar to typical carbonaceous chondrites, and distinct from ordinary or enstatite chondrites. The similar mean of ¹⁸⁷Os/¹⁸⁸Os measured for the ureilites and carbonaceous chondrites suggests that the ureilite parent body probably formed within the same region of the solar nebula as carbonaceous chondrites. From the narrow range of the ¹⁸⁷Os/¹⁸⁸Os distribution in ureilite meteorites it is further concluded that Re was not significantly fractionated from Os during planetary differentiation and was not lost along with the missing ureilitic melt component. The lack of large Re/Os fractionations requires that Re/Os partitioning was controlled by a metal phase, and thus metal had to be stable throughout the interval of magmatic processing on the ureilite parent body.