中子俘获元素的原子数据进展
Advances in Atomic Data for Neutron-Capture Elements
摘要：
在近100颗行星状星云中探测到了中子俘获元素（原子序数Z>30），它们可以在行星状星云（PN）的祖星中通过s-过程核合成产生。这表明星云光谱学是研究反式铁元素的产生和化学演化的一个潜在的强有力的工具。然而，在实现这一目标之前，必须应对重大挑战。最大的障碍之一是缺乏n-捕获元素的原子数据，特别是需要解决它们的电离平衡（从而将离子丰度转换为元素丰度）。为了解决这个问题，我们计算了光电离截面和辐射和双电子复合速率系数的前六个离子的硒和氪。计算基准对实验光电离截面测量。此外，我们计算了电荷转移（CT）率系数的离子的六个N-捕获元素。这些努力将使星云的硒和氪丰度的准确测定，允许强大的调查的S-过程富集PNE。
英文摘要：
Neutron(n)-capture elements (atomic number Z>30), which can be produced in planetary nebula (PN) progenitor stars via s-process nucleosynthesis, have been detected in nearly 100 PNe. This demonstrates that nebular spectroscopy is a potentially powerful tool for studying the production and chemical evolution of trans-iron elements. However, significant challenges must be addressed before this goal can be achieved. One of the most substantial hurdles is the lack of atomic data for n-capture elements, particularly that needed to solve for their ionization equilibrium (and hence to convert ionic abundances to elemental abundances). To address this need, we have computed photoionization cross sections and radiative and dielectronic recombination rate coefficients for the first six ions of Se and Kr. The calculations were benchmarked against experimental photoionization cross section measurements. In addition, we computed charge transfer (CT) rate coefficients for ions of six n-capture elements. These efforts will enable the accurate determination of nebular Se and Kr abundances, allowing robust investigations of s-process enrichments in PNe.
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