Qian Y
Astrophys J. 2000 May 1;534(1):L67-L70. doi: 10.1086/312659.
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.
我表明，如果中子星合并（NSM）是主要的r过程源，那么近期对贫金属恒星中r过程丰度的观测结果将难以解释。相比之下，早期太阳系中关于182Hf和129I的此类观测以及陨石数据支持了超新星（SNe）进行r过程富集的自洽图景。虽然对于超新星和中子星合并，r过程产生和富集都需要进一步的理论研究，但我强调超新星r过程模型的两个可能的直接观测检验：超新星遗迹中r过程核衰变产生的伽马射线，以及双星中超新星r过程抛射物对伴星表面的污染。
