论文标题
中子星合并可以单独解释银河系的R-过程吗？
Can neutron star mergers alone explain the r-process enrichment of the Milky Way?
论文作者
论文摘要
将银河化学演化模型与以银河系的观察到的元素丰度进行比较，我们表明，只有当在低金属金属率下，中子恒星合并才能成为领先的R-process位点，这些合并具有很短的延迟时间和大量的喷射质量，这些质量是由紧凑物体的质量促进的。也就是说，根据黑洞的旋转，黑洞中的星星合并在银河系的早期化学富集中起着重要作用。我们还表明，本文中使用的二元种群综合模型均未使用，即Compas，Startrack，Brussels，组合和BPASS，目前都无法再现元素丰度观察。这些预测不仅对中子星的合并是有问题的，而且对于IA型超新星而言，这可能表明二进制进化模型中的缺点。
Comparing Galactic chemical evolution models to the observed elemental abundances in the Milky Way, we show that neutron star mergers can be a leading r-process site only if at low metallicities such mergers have very short delay times and significant ejecta masses that are facilitated by the masses of the compact objects. Namely, black hole-neutron star mergers, depending on the black-hole spins, can play an important role in the early chemical enrichment of the Milky Way. We also show that none of the binary population synthesis models used in this paper, i.e., COMPAS, StarTrack, Brussels, ComBinE, and BPASS, can currently reproduce the elemental abundance observations. The predictions are problematic not only for neutron star mergers, but also for Type Ia supernovae, which may point to shortcomings in binary evolution models.
