发表机构
School of Physics and Astronomy, University of Minnesota; Theoretical Division and Center for Theoretical Astrophysics, Los Alamos National Laboratory; GSI Helmholtzzentrum für Schwerionenforschung（明尼苏达大学物理与天文学学院; 洛斯阿拉莫斯国家实验室理论部与理论天体物理中心; GSI亥姆霍兹重离子研究中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究基于68颗贫金属恒星的元素丰度，提出覆盖Sr到U的r-过程生产模式的数据驱动模型，发现r-过程模式可由模式1和2混合解释，明确两类模式的来源，强调需进一步测量以完善模型。
AI 中文摘要
利用68颗贫金属（MP）恒星中的元素丰度，我们提出了一种覆盖从锶（Sr）到铀（U）的r-过程生产模式的数据驱动模型。我们表明，这些恒星及其他测试恒星中几乎所有的r-过程模式都可以通过模式1和模式2的混合来充分解释，这为有限r、r-I和r-II恒星的经验分类提供了理论见解。我们对参数化r-过程计算产生的产额模板进行了广泛调查。我们提出，模式2可能由单一模板主导，指向一部分中子星并合（NSMs）产生的r-过程的规律性，而模式1是多个模板的平均叠加，反映了其他NSMs以及可能的一些磁旋转超新星的生产。我们指出了不同电离状态下测量的元素丰度比可能存在的系统问题，并强调需要检查HD 122563的锇（Os）、铱（Ir）和铂（Pt）测量值，根据我们的模型，该恒星以模式1为主，具有显著的Pt峰。如果这一结果得到证实，有限r类别的含义需要进行重大修正。对更大样本的MP恒星中更广泛范围的r-过程元素进行进一步测量，对于测试和改进我们的模型至关重要。
英文摘要
Using the elemental abundances in 68 metal-poor (MP) stars, we present a data-driven model for $r$-process production patterns covering Sr to U. We show that essentially all the $r$-process patterns in those and other test stars can be adequately explained as mixtures of Patterns 1 and 2, which provides theoretical insights into the empirical categories of limited-$r$, $r$-I, and $r$-II stars. We carry out an extensive survey of the yield templates produced by parametric $r$-process calculations. We propose that Pattern 2 may be dominated by a single template and points to regularity in $r$-process production by a subset of neutron star mergers (NSMs), while Pattern 1 is the average superposition of multiple templates and reflects production by other NSMs and perhaps also some magneto-rotational supernovae. We raise possible systematic issues with abundance ratios for elements measured in different ionization states, and highlight the need for examining the Os, Ir, and Pt measurements for HD~122563, which is dominated by Pattern 1 with a prominent Pt peak in our model. If this result is confirmed, the meaning of the limited-$r$ category requires drastic revision. Further measurements of a wider range of $r$-process elements in a larger sample of MP stars are critical to test and improve our model.
Comments48 pages; published in The Astrophysical Journal (ApJ)
Journal refAstrophys. J. 1010, 35 (2026)
