Supernovae versus Neutron Star Mergers as the Major r-Process Sources
Supernovae versus Neutron Star Mergers as the Major r-Process Sources
复制标题
超新星与中子星合并作为主要的 r 过程源
DOI：
10.1086/312659
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发表时间：
2000
期刊：
影响因子：
--
通讯作者：
Y. Qian
中科院分区：
文献类型：
--
作者：
Y. Qian
我表明，如果中子星合并（nsm）是主要的r过程源，那么最近对金属贫恒星中r过程丰度的观测很难解释。相比之下，这些观测和早期太阳系中182Hf和129I的陨石数据支持超新星（SNe） r过程富集的自一致图像。虽然SNe和NSMs都需要进一步的r过程产生和富集的理论研究，但我强调了SN r过程模型的两个可能的直接观测测试：SN残余物中r过程核衰变的伽马射线和双星中SN r过程抛射物对伴星表面的污染。
I show that recent observations of r-process abundances in metal-poor stars are difficult to explain if neutron star mergers (NSMs) are the major r-process sources. In contrast, such observations and meteoritic data on 182Hf and 129I in the early solar system support a self-consistent picture of r-process enrichment by supernovae (SNe). While further theoretical studies of r-process production and enrichment are needed for both SNe and NSMs, I emphasize two possible direct observational tests of the SN r-process model: gamma rays from the decay of r-process nuclei in SN remnants and surface contamination of the companion by SN r-process ejecta in binaries.