r-Process in Neutron Star Mergers
r-Process in Neutron Star Mergers
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DOI：
10.1086/312343
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发表时间：
1999-11
期刊：
影响因子：
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通讯作者：
C. Freiburghaus;S. Rosswog;F. Thielemann
中科院分区：
文献类型：
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作者：
C. Freiburghaus;S. Rosswog;F. Thielemann
尽管进行了大量研究，但通过快速中子俘获（r过程）形成的富中子重元素的产生地点仍然未知。在这里，我们展示了对 Lattimer & Schramm、Symbalisty & Schramm、Eichler 等人和 Davies 等人早期提出的场景的详细研究，即两颗中子星的合并。结合流体动力学和全网络计算的结果，以研究该场景与 r 过程核合成的相关性。通过中子星物质的减压，喷射出足够的物质来解释银河系中r过程核的数量。假设喷射物由质子与核子之比为 Ye ≈ 0.1 的物质组成，对于包含 A ≈ 130 峰且重于 A ≈ 130 峰的核，计算出的丰度非常适合观测到的太阳 r 模式。
The production site of the neutron-rich heavy elements that are formed by rapid neutron capture (the r-process) is still unknown despite intensive research. Here we show detailed studies of a scenario that has been proposed earlier by Lattimer & Schramm, Symbalisty & Schramm, Eichler et al., and Davies et al., namely the merger of two neutron stars. The results of hydrodynamic and full network calculations are combined in order to investigate the relevance of this scenario for r-process nucleosynthesis. Sufficient material is ejected to explain the amount of r-process nuclei in the Galaxy by decompression of neutron star material. Provided that the ejecta consist of matter with a proton-to-nucleon ratio of Ye ≈ 0.1, the calculated abundances fit the observed solar r-pattern excellently for nuclei that include and are heavier than the A ≈ 130 peak.