...
  • 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>Earth and Planetary Science Letters: A Letter Journal Devoted to the Development in Time of the Earth and Planetary System >Formation of solar nebula reservoirs by mixing chondritic components
【24h】

Formation of solar nebula reservoirs by mixing chondritic components

机译：通过混合软骨成分形成太阳星云储层

获取原文
获取原文并翻译 | 示例
           
页面导航
  • 摘要
  • 著录项
  • 相似文献
  • 相关主题

摘要

We determined proportions of Type 1 (reduced) and Type 11 (oxidized) chondrules in ordinary chondrites (OC) and found linear relationships between chondrule abundances and chondrite bulk chemical and oxygen isotopic compositions. Similar relationships exist between bulk oxygen isotopic compositions of carbonaceous chondrites and modal abundances of their chondritic components (matrix, Type 1 and Type 11 chondrules, refractory calcium-aluminium-rich inclusions and amoeboid olivine aggregates). These correlations can be used to predict the bulk oxygen isotopic composition of chondrites based on their petrology. We can also define model isotopic compositions associated with each petrologic component, which are not their current actual isotopic compositions due to alteration or mixing. These compositions for refractory inclusions and chondrules plot close to a slope I line, consistent with refractory inclusions (RI) forming from an early O-16-rich gas, the evolution of the gas to more O-16-poor compositions, possibly involving photodissociation and subsequent ice transport, followed by chondrule formation. Our results open a new understanding of the oxygen 3-isotope space and explain the unique position of OC as well as the differences between H, L and LL chondrites. They indicate that major chemical and isotopic variations between chondritic reservoirs were established after chondrule and CAI formation. They may have some bearing on the formation of planetary reservoirs: the Delta O-17 calculated for type I chondrules is appropriate for terrestrial planet progenitors, consistent with their chemical similarity to Earth mantle. (c) 2006 Elsevier B.V. All rights reserved.
机译：我们确定了普通球粒（OC）中1型（还原）和11型（氧化）球粒的比例，并发现了球粒丰度与球粒体化学和氧同位素组成之间的线性关系。碳质球粒陨石的大量氧同位素组成与其软骨成分的模态丰度（基质，1型和11型球粒，难熔的钙铝富集夹杂物和类变形橄榄石聚集体）之间存在相似的关系。这些相关性可用于根据球石的岩石学预测球粒陨石的总氧同位素组成。我们还可以定义与每个岩石学成分相关的模型同位素组成，由于改变或混合，它们不是当前的实际同位素组成。这些用于难熔夹杂物和软骨的组合物的图线接近I线，这与早期富含O-16的气体形成难熔夹杂物（RI），气体演化为贫O-16的组合物（可能涉及光解离）相一致。然后进行冰运输，然后形成软骨。我们的研究结果使人们对氧3同位素空间有了新的认识，并解释了OC的独特位置以及H，L和LL球粒陨石之间的差异。他们表明，软骨和CAI形成后，在软骨储层之间建立了主要的化学和同位素变化。它们可能与行星储层的形成有关：为I型软骨计算的Delta O-17适用于陆地行星祖细胞，这与它们与地幔的化学相似性相一致。 （c）2006 Elsevier B.V.保留所有权利。

著录项

相似文献

  • 外文文献
  • 中文文献
  • 专利
获取原文

客服邮箱：kefu@zhangqiaokeyan.com

京公网安备：11010802029741号 ICP备案号：京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有

  • 客服微信

  • 服务号