热恒星内部能量的原始e -俘获截面

P. Giannaka, T. Kosmas, H. Ejiri
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引用次数: 1

摘要

核电子俘获反应在爆炸核合成过程中,特别是在大质量恒星演化的后期,具有突出的地位。在这项工作中,我们使用质子-中子(pn)准粒子随机相位近似对绝对e -捕获横截面进行了排他计算。因此,本研究的结果可以作为在相同条件下进行的实验的预测,并用于探索大质量恒星的前超新星和超新星阶段的恒星环境中e-捕获过程的作用。我们研究的主要目标是提供一组铁族原子核(28Si, 32S, 48Ti, 56Fe, 66Zn和90Zr)周围同位素的e-捕获的原始截面的详细计算,这些同位素在超新星前和核心坍缩超新星阶段在能量范围0≤e≤50 MeV内发挥重要作用。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Original e− Capture Cross Sections for Hot Stellar Interior Energies
The nuclear electron capture reaction possesses a prominent position among other weak interaction processes occurring in explosive nucleosynthesis, especially at the late stages of evolution of massive stars. In this work, we perform exclusive calculations of absolute e−-capture cross sections using the proton–neutron (pn) quasi-particle random phase approximation. Thus, the results of this study can be used as predictions for experiments operating under the same conditions and in exploring the role of the e−-capture process in the stellar environment at the pre-supernova and supernova phase of a massive star. The main goal of our study is to provide detailed state-by-state calculations of original cross sections for the e−-capture on a set of isotopes around the iron group nuclei (28Si, 32S, 48Ti, 56Fe, 66Zn and 90Zr) that play a significant role in pre-supernova as well as in the core–collapse supernova phase in the energy range 0≤E≤50 MeV.
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