硼天体化学。第二部分:硼核合成和缩合温度

Mingzhe Zhai
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引用次数: 11

摘要

-由Zhai和Shaw(1994)计算的新的B太阳系丰度,16.9个原子/106 Si(或606个原子/1012 H)用于重新评估LiBeB (7Li除外)核合成的不同可能性。修正后的丰度支持两个模型:(1)轻元素是由星系宇宙射线(GCRs)对星际介质(ISM)的持续轰击形成的,但这些星系宇宙射线应该包含一个非常强烈的低能成分,其形式为E - 5,由于太阳调制效应,在地球附近无法观测到;(2)轻元素是两个光源的混合物。在第一个来源中,轻元素是由星系宇宙射线不断轰击星际介质合成的。在第二种来源中,它们是由超新星喷出的C和O原子核与周围气体中的H和He相互作用产生的。碳质球粒陨石中常见元素和挥发性元素的si归一化丰度和ci陨石归一化丰度与它们的冷凝温度呈线性相关。利用这一关系和CM、CO和CV陨石中归一化的B丰度,我们可以估计出B的冷凝温度为~ 910 K,与Ga相似。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Boron cosmochemistry. Part II: Boron nucleosynthesis and condensation temperature
— The new B solar-system abundance calculated by Zhai and Shaw (1994), 16.9 atoms/106 Si (or 606 atoms/1012 H) is used to reevaluate the different possibilities of LiBeB (except 7Li) nucleosynthesis. The revised abundances support two models: (1) Light elements were formed by continual bombardment of interstellar medium (ISM) by galactic cosmic rays (GCRs), but these galactic cosmic rays should contain a very intense low-energy component, in the form of E−5 which cannot be observed near the Earth due to solar modulation effects; (2) Light elements are a mixture of two sources. In the first source, light elements were synthesized by continual bombardment of interstellar medium by galactic cosmic rays. In the second source, they were made by the interactions of C and O nuclei ejected from supernovae with the H and He in the surrounding gas. The first source constitutes ∼46% of total B. The Si-normalized and CI-meteorite-normalized abundances of common and volatile elements in carbonaceous chondrites show a linear correlation with their condensation temperatures. Using this relationship and the normalized B abundances in CM, CO, and CV meteorites, we can estimate the B condensation temperature to be ∼910 K, which is similar to Ga.
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