Noble Gases in Meteorites – Trapped Components
Noble Gases in Meteorites – Trapped Components
复制标题
陨石中的稀有气体 - 被捕获的成分
DOI：
10.2138/rmg.2002.47.3
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发表时间：
2002
影响因子：
--
通讯作者：
U. Ott
中科院分区：
文献类型：
--
作者：
U. Ott
宇宙化学领域的基本见解来自于对被困惰性气体的丰度和同位素组成的研究。一个恰当的例子是在原始陨石中发现太阳前颗粒：在发现纳米金刚石、碳化硅和石墨等太阳前颗粒之前很久就知道惰性气体中的同位素丰度异常，正是对这些异常的载体相的寻找最终导致了这些类型颗粒的识别和分离（例如，Anders and Zinner 1993; Ott 1993）。
从约翰·雷诺兹（John Reynolds）和他在伯克利的同事们的工作开始，许多关于惰性气体的工作都集中在氙上，以至于创造了一个自己的术语“氙学”（xenology）来描述惰性气体宇宙化学的这一领域（Reynolds 1963）。第一个所谓的“富含气体的陨石”是在1956年由俄罗斯工作人员发现的（Gerling和Levskii 1956），同年雷诺兹发表了他创新的静态惰性气体质谱仪的细节（Reynolds 1956）。此后不久，人们发现，在陨石中观察到的元素丰度模式基本上分为两种模式之一：（a）富含气体的陨石，具有“太阳”模式-与重气体相比，最轻气体He和Ne的丰度较高，其来源是注入的太阳风;（B）具有强烈元素分馏的“行星”模式，即，与太阳丰度模式相比，重惰性气体相对于轻惰性气体的富集程度更高（Signer和Suess，1963;图1）。“行星”气体在最原始的碳质玄武岩中最为丰富（Marti 1967; Mazor等人1970）。在本章中，我将专门讨论陨石中的稀有气体类型，这些气体包括在最初定义的“行星成分”中。太阳风惰性气体也是...
Fundamental insights in the field of cosmochemistry have come from the study of the abundances and isotopic compositions of trapped noble gases. A case in point is the discovery of presolar grains in primitive meteorites: isotope abundance anomalies in noble gases were known long before the discovery of presolar grains such as nanodiamonds, silicon carbide and graphite, and it was the search for the carrier phases of these anomalies that ultimately led to the identification and isolation of these types of grains (e.g., Anders and Zinner 1993; Ott 1993).
Starting with the work of John Reynolds and his colleagues at Berkeley, much of the work on trapped noble gases has centered on xenon, so much that an own term “xenology” was coined to describe this field of noble gas cosmochemistry (Reynolds 1963). The first of the so-called “gas-rich meteorites” were discovered by Russian workers in 1956 (Gerling and Levskii 1956), the same year that Reynolds published details of his innovative static noble gas mass spectrometer (Reynolds 1956). Soon thereafter it was discovered that the elemental abundance patterns observed in meteorites basically fell into one of two patterns: (a) the gas-rich meteorites with a “solar” pattern—high abundances of the lightest gases He and Ne compared to the heavy ones, the origin being implanted solar wind; and (b) the “planetary” pattern with strong elemental fractionation, i.e., strong enrichment of the heavy noble gases relative to the light ones, when compared to the solar abundance pattern (Signer and Suess 1963; Fig. 1⇓). “Planetary” gases are most abundant in the most primitive carbonaceous chondrites (Marti 1967; Mazor et al. 1970). In this chapter I will deal exclusively with the type of noble gases in meteorites included in the “planetary component” as originally defined. Solar wind noble gases as well …