Reanalysis of the Isotopic Mixture of Neutron-Capture Elements in the Metal-Poor Star HD 175305
Reanalysis of the Isotopic Mixture of Neutron-Capture Elements in the Metal-Poor Star HD 175305
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DOI：
10.1088/0256-307x/29/1/019701
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发表时间：
2012-02
影响因子：
3.5
通讯作者：
Jiang Zhang;Bo Wang;Bo Zhang;Zhangang Han
中科院分区：
文献类型：
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作者：
Jiang Zhang;Bo Wang;Bo Zhang;Zhangang Han
传统上认为，中子捕获过程是Fe以外重元素核合成的原因。基于最小二乘法和太阳同位素丰度的经典模型，我们估计的相对贡献的s-和r-过程的中子捕获元素的丰度在贫金属星星HD 175305的分量系数。应用计算的组分系数Cr和Cs，模型预测了Nd、Sm和Eu的同位素分数分别为f142+144 = 0.482、f152+154 = 0.525和f151 = 0.450。以及所观察到的丰度，各向同性分数也与计算一致。最后，我们第一次从HD 175305中不同元素的同位素分数估计了两个中子过程（r-和s-过程）的贡献百分比，例如Sm的4604 π线的r-过程贡献为67%+21%−32%。
The neutron-capture process is traditionally postulated to be responsible for the nucleosynthesis of heavy elements beyond Fe. Based on the least squares method and solar isotopic abundances from the classical model, we estimate the relative contributions of the s- and r-processes to the abundance of neutron-capture elements in the metal-poor star HD 175305 from the component coefficients. Applying the calculated component coefficients Cr and Cs, the model predicts the isotopic fractions of elements Nd, Sm and Eu to be f142+144 = 0.482, f152+154 = 0.525 and f151 = 0.450, respectively. As well as the observed abundances, the isotropic fractions are also consistent with the calculations. Finally, for the first time, we estimated the contribution percentage of the two neutron processes (the r- and s-processes) from the observed isotopic fractions of different elements in HD 175305, e.g. an r-process contribution of 67%+21%−32% from the 4604 Å line of Sm.