Nucleosynthesis in Supernova Shock Waves
Nucleosynthesis in Supernova Shock Waves
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DOI：
10.1139/p67-184
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发表时间：
1967-07
影响因子：
1.2
通讯作者：
J. Truran;W. D. Arnett;A. Cameron
中科院分区：
文献类型：
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作者：
J. Truran;W. D. Arnett;A. Cameron
人们普遍认为，在超新星爆炸中存在的极端条件下，元素合成很容易发生。我们研究了通过恒星包层传播的超新星冲击波中可能发生的热核反应的类型，其中温度可能会持续约 10−2 秒，约为 5 × 109 °K。计算是使用通过吸收或发射中子、质子、α粒子和光子而与其邻居相连的原子核网络来执行的（Truran et al. 1966）。结果表明，超新星冲击波可以产生铁峰元素，但除非在冲击波通过之前材料中发生了某种质子向中子的转变，否则不会产生自然界中观察到的铁峰成分。此外，在这些条件下，恒星包层中无法获得足以驱动快速中子俘获过程的中子通量。
It is generally assumed that element synthesis will take place readily under the extreme conditions believed to exist in supernova explosions. We have examined the types of thermonuclear reactions that can occur in a supernova shock wave which propagates through the stellar envelope, in which a temperature ~5 × 109 °K may occur for ~10−2 seconds. The calculations are performed using a network of nuclei connected to their neighbors by absorption or emission of neutrons, protons, alpha particles and photons (Truran et al. 1966). The results show that iron-peak elements can be produced by a supernova shock wave, but the iron-peak composition observed in nature is not produced unless some transformation of protons to neutrons has taken place in the material before the passage of the shock wave. Furthermore, a neutron flux sufficient to drive the rapid neutron-capture process is not attained under these conditions in the stellar envelope.