Possibility to Identify the Contributions from Collapsars, Supernovae, and Neutron Star Mergers from the Evolution of the r-process Mass Abundance Distribution
Possibility to Identify the Contributions from Collapsars, Supernovae, and Neutron Star Mergers from the Evolution of the r-process Mass Abundance Distribution
复制标题
DOI：
10.3847/1538-4357/ac721c
复制
发表时间：
2022-07
期刊：
影响因子：
--
通讯作者：
Y. Yamazaki;Zhenyu He;T. Kajino;G. Mathews;M. Famiano;Xiao-Dong Tang;Jian-rong Shi
中科院分区：
文献类型：
--
作者：
Y. Yamazaki;Zhenyu He;T. Kajino;G. Mathews;M. Famiano;Xiao-Dong Tang;Jian-rong Shi
我们研究星系中快速中子俘获过程（r 过程）同位素的演化。我们分析了一系列天体物理条件和核输入数据下核心塌缩超新星（CCSNe）、中子星合并和塌缩星的相对贡献。在这里，我们表明，尽管每个位点的 r 过程都可以导致相似的（普遍）元素分布，但不同位点的详细同位素丰度可能不同。这些差异可能有助于识别哪些来源促成了星系中 r 过程物质的早期演化。我们的模拟表明，早期演化主要由 CCSNe 和塌缩星 r 过程核合成主导。如果下一代天文台能够推导出同位素 r 过程丰度，那么这个结论可能是可检验的。
We study the evolution of rapid neutron-capture process (r-process) isotopes in the galaxy. We analyze relative contributions from core-collapse supernovae (CCSNe), neutron star mergers, and collapsars under a range of astrophysical conditions and nuclear input data. Here we show that, although the r-process in each of these sites can lead to a similar (universal) elemental distribution, the detailed isotopic abundances can differ from one site to another. These differences may allow for the identification of which sources contributed to the early evolution of r-process material in the galaxy. Our simulations suggest that the early evolution was dominated by CCSNe and collapsar r-process nucleosynthesis. This conclusion may be testable if the next generation of observatories can deduce isotopic r-process abundances.