AI 中文总结
该研究通过随机混合模型拟合晕星元素丰度，发现正常核心坍缩超新星与中子星并合的组合比磁旋转超新星更符合观测结果，消除了磁旋转超新星作为丰度来源的证据。
AI 中文摘要
近期一项研究声称，通过将晕星观测到的元素丰度模式与单次超新星/超新星爆发事件的总产额拟合，仅磁旋转超新星（一种也会产生r过程元素的高能超新星事件）可作为观测丰度的来源。本文表明，在混合随机性框架下，结合正常核心坍缩超新星（ccSN；爆发能量$_{\rm exp}$约为$10^{51}$ erg）与中子星并合（NSM）的产额，能更好地拟合该恒星的特殊丰度模式。随机混合模型的拟合效果显著优于超新星拟合，均方根误差为0.24，而超新星拟合的均方根误差为0.44，即相较于磁旋转超新星场景，该模型更支持常见事件（ccSN + NSM）的成分。本文还讨论了该恒星的起源，以及其诞生云被ccSN和NSM共同增丰的可能性。
英文摘要
A recent work claimed by fitting the observed elemental abundance pattern of a halo star with the total yields from single super-/hypernova events that only a magnetorotational hypernova event (a very energetic supernova event that also produces r-process elements) could be the source of the observed abundances. Here, we show that the star's peculiar abundance pattern is better fitted within the framework of mixing stochasticity with yields from a normal core collapse supernova (ccSN; Energy$_{\rm exp}$ $\sim 10^{51}$ erg.) and a neutron star merger (NSM). The stochastic mixing model outperforms the hypernova fitting significantly, (r.m.s 0.24 vs 0.44) i.e., favours the composition from common events (ccSN + NSM) over the magnetorotational hypernova scenario. We also discuss the origin of the star and the possibility of enrichment of its birth cloud by both a ccSN and a NSM.
Comments7 Pages, 3 Figures, 3 Tables, accepted for publication in MNRAS Letters
