Abundances and distribution of volatile trace elements in chondritic meteorites and their components

内太阳系的行星和小行星的挥发性元素，如Na， K， Zn和Cd的消耗是有限的。这种消耗的原因是无限制的。挥发性元素的不完全冷凝被广泛认为是造成普遍的原始耗竭的原因，但也提出了其他模型，如球粒形成过程中的耗竭或来自星际介质（ISM）的继承。原始挥发性元素耗损的记录被后来明显的挥发性元素再分配过程所模糊，例如在富Ca、富Al包裹体（CAIs）或普通球粒陨石中。本研究的目标是通过对关键样品应用复杂的分析技术来限制导致早期太阳系材料中挥发性元素耗尽和再分配的过程：i)首次对块状球粒陨石及其组分（球粒，基质，CAIs）中的挥发性元素进行高精度同位素稀释分析；ii)通过激光烧蚀ICP-MS研究球粒陨石中挥发性元素的微分布。

Planets and asteroids of the inner solar system are depleted in volatile elements such as Na, K, Zn and Cd. The cause of this depletion is unconstrained. Incomplete condensation of volatile elements is widely thought to be responsible for the pervasive primary depletion, but alternative models such as depletion during chondrule formation or inheritance from the interstellar medium (ISM) have been proposed. The record of primary volatile element depletion is blurred by later volatile element redistribution processes that is evident, e.g., in Ca, Al rich inclusions (CAIs) or ordinary chondrites.The goal of this study is to constrain the processes that led to the depletion and redistribution of volatile elements in early solar system materials by the application of sophisticated analytical techniques to key samples: i) the first high-precision isotope dilution analyses of volatile elements in bulk chondrites and their components (chondrules, matrix, CAIs) and ii) the study of the microdistribution of volatile elements in chondrites by laser ablation ICP-MS.