我国南极陨石研究的新进展

近年来,因在南极发现了大量的陨石样品,我国天体化学和陨石学研究得到了快速发展,并取得了一系列可喜的成果,如:①在南极已收集了近万块南极陨石样品,使我国已成为南极陨石拥有大国;②大量的陨石发现和研究成果表明格罗夫山地区为我国发现的新的陨石富集区,填补了我国在南极陨石领域的空白;③发现了许多我国奇缺的陨石类型,如火星陨石、CR型碳质球粒陨石等;④开展了较深入的CAI研究等.这些都将为我国天体化学和比较行星学的发展展示广阔的前景.提出了一些南极陨石研究工作中存在的问题和今后的工作方向.     

Chemical Analysis of Iron Meteorites Using a Hand‐Held X‐Ray Fluorescence Spectrometer

We evaluate the performance of a hand‐held XRF (HHXRF) spectrometer for the bulk analysis of iron meteorites. Analytical precision and accuracy were tested on metal alloy certified reference materials and iron meteorites of known chemical composition. With minimal sample preparation (i.e., flat or roughly polished surfaces) HHXRF allowed the precise and accurate determination of most elements heavier than Mg, with concentrations > 0.01% m/m in metal alloy CRMs, and of major elements Fe and Ni and minor elements Co, P and S (generally ranging from 0.1 to 1% m/m) in iron meteorites. In addition, multiple HHXRF spot analyses could be used to determine the bulk chemical composition of iron meteorites, which are often characterised by sulfide and phosphide accessory minerals. In particular, it was possible to estimate the P and S bulk contents, which are of critical importance for the petrogenesis and evolution of Fe‐Ni‐rich liquids and iron meteorites. This study thus validates HHXRF as a valuable tool for use in meteoritics, allowing the rapid, non‐destructive (a) identification of the extraterrestrial origin of metallic objects (i.e., archaeological artefacts); (b) preliminary chemical classification of iron meteorites; (c) identification of mislabelled/unlabelled specimens in museums and private collections and (d) bulk analysis of iron meteorites.     

陨石Cr同位素组成测试技术及其在天体化学研究中的应用

Cr同位素作为一个新的研究手段,在天体化学领域中主要应用于追溯太阳系早期历史演化和定年.Cr同位素组成测定的主要技术是二次离子探针、热电离质谱和多接收等离子质谱,本文对这些分析技术的特点和发展作了论述.随着分析技术的发展,目前对ε(53Cr)和ε(54Cr)测定精度分别达到6 ppm和12 ppm(2σ).高精度Cr同...     

离子探针测试方法及其在矿物微区微量元素和同位素分析中的应用

离子探针能在单矿物颗粒内进行微区原位直接分析工作,主离子束斑大小可聚焦在5μm以内,可以检测到10^-9级的微量元素,同位素分析的精度高达1‰,在地球科学领域有着广泛的应用。详细叙述了离子探针的工作原理以及微量元素成分和同位素组成的测试方法,列举了其在天体化学和地球化学研究领域的主要应用,总结了一系列的研究成果,并首次公开发表离子探针微量元素测试技术研发工作中取得的一些实验结果。     

天体化学:地球起源与演化的几个关键问题

以近几年天体化学研究取得的一些重要成果，论述了对于认识地球的起源和演化进程的重要意义。地球主要由一套具有独立化学成分组成的硅酸盐质星子群随机碰撞吸积而成。地球的星子堆积形成方式和初始化学成分的不均一性制约着地球后期的非均一、非均变演化过程。以１８００Ｍａ为转折点，地球的演化具明显的两阶段演化特征：早期以初生壳体———星子源地体的形成和发展为特点，后期以岩石圈板块运动为特点。地球演化史中的地外撞击事件，是太阳系形成机制———碰撞吸积作用的继续，是地质历史生物、沉积、岩浆、构造等演化的重要营力之一。     

太阳系形成及演化研究方法

通过对陨石的研究,说明太阳系的形成与演化历史,包括太阳星云的凝聚过程、高温加热熔融事件和低温蚀变过程,陨石母体的热变质作用、熔融分异作用以及冲击变质作用等。对太阳星云的化学组成和同位素组成不均一性、前太阳物质的存在及其意义、太阳系形成和演化的同位素绝对年龄、间隔年龄以及宇宙射线暴露年龄等进行了讨论。结合太阳系形成和演化的研究,特别对电子探针、离子探针、透射电子显微镜以及拉曼光谱等微束分析技术在该领域的应用和相关问题进行了讨论。     

强亲铁元素高温地球化学与天体化学及研究进展

强亲铁元素(HSE)包括铂族元素(PGE):Os、Ir、Ru、Rh、Pt、Pd)及Re、Au,它们对金属与硫化物相具有强烈的亲和性,这种独特性质使其成为高温地球化学与天体化学研究中的优秀示踪剂。此外,强亲铁元素内含两种长半衰期(¹⁸⁷Re-¹⁸⁷Os,t_1/2=41.6 Ga;¹⁹⁰Pt-¹⁸⁶Os,t_1/2=469 Ga)和一种短半衰期(¹⁰⁷Pd-¹⁰⁷Ag,t_1/2=6.5 Ma)放射性同位素衰变体系,可以用作地球与天体演化的时钟。在地幔部分熔融或分离结晶期间,PPGE(Rh、Pd、Pt)与Re、Au倾向于进入熔体相,IPGE(Os、Ir、Ru)则更多保留在残余固相。因此,通过地幔包体、地幔构造岩、镁铁质与超镁铁质火山岩的HSE丰度与Os同位素可约束地幔组成和相应的岩浆过程,以及制约地球早期演化过程。随着分析技术的改进,HSE与Re-Pt-Os同位素在行星增生与分异、核幔相互作用、壳幔分异、洋陆转换、克拉通形成与破坏、岩石圈俯冲再循环以及Ni-Cu-PGE矿床成因等方面均显示了巨大的应用潜力。     

Zirconium isotope evidence for incomplete admixing of r-process components in the solar nebula

Isotopic anomalies in Mo and Zr have recently been reported for bulk chondrites and iron meteorites and have been interpreted in terms of a primordial nucleosynthetic heterogeneity in the solar nebula. We report precise Zr isotopic measurements of carbonaceous, ordinary and enstatite chondrites, eucrites, mesosiderites and lunar rocks. All bulk rock samples yield isotopic compositions that are identical to the terrestrial standard within the analytical uncertainty. No anomalies in ⁹²Zr are found in any samples including high Nb/Zr eucrites and high and low Nb/Zr calcium-aluminum-rich inclusions (CAIs). These data are consistent with the most recent estimates of <10⁻⁴ for the initial ⁹²Nb/⁹³Nb of the solar system. There exists a trace of isotopic heterogeneity in the form of a small excess of r-process ⁹⁶Zr in some refractory CAIs and some metal-rich phases of Renazzo. A more striking enrichment in ⁹⁶Zr is found in acetic acid leachates of the Allende CV carbonaceous chondrite. These data indicate that the r- and s-process Zr components found in presolar grains were well mixed on a large scale prior to planetary accretion. However, some CAIs formed before mixing was complete, such that they were able to sample a population of r-process-enriched material. The maximum amount of additional r-process component that was added to the otherwise well-mixed Zr in the molecular cloud or disk corresponds to ∼0.01%.