论文标题
对流的H-HE相互作用在大量人群III恒星进化模型中
Convective H-He Interactions in Massive Population III Stellar Evolution Models
论文作者
论文摘要
在POP III恒星模型中，对流诱导的H-和HE富燃烧层之间的混合可以诱导一连串的核能，从而大大改变了第一批大型恒星中随后的进化和核合成。我们使用五组混合假设，研究了26个恒星演化模拟中的H shell和核心交互作用，$ 15-140 \，\ mathrm {m} _ {\ odot} $，使用五组混合假设。在22个情况下，H -HE相互作用在范围内诱导局部核能发布$ \ sim 10^{9} -10^{13.5} \，\ Mathrm {l} _ {\ odot} $。该范围的上端的亮度在对流的对流时间尺度上相当于该层的内部能量的很大一部分，表明动态恒星响应将违反1D恒星进化建模假设。我们根据富含他富含的材料的进化阶段和对流稳定性来区分四种类型的H-HE相互作用。 H-H-H-HE交互过程中的H燃烧条件给出$^{12} \ MATHRM {C}/^{13} \ MATHRM {C} $比率在$ \ $ \ $ \ $ \ $ \ sim 1000 $和[C/N]的比例约为$ \ y $ \ collelelations and corlelations and collelations and corlations and colle plans collations and colle and collations and colle plancep，我们还从热CNO突破中探索了CA的产生，发现此处提供的模拟可能无法解释观察到的CA丰度在最糟糕的CEMP-NO恒星中。我们描述了导致H-HE相互作用的演化，该进化发生在核心量子阶段之后或不久之后。三个没有H-HE相互作用的模拟计算为Fe-core Inclall，$ 140 \，\ Mathrm {M} _ {\ odot} $仿真变为PAIR-UNSTABLE。我们还讨论了当前的建模局限性以及3D流体动力学模型的需求，以充分了解这些恒星进化阶段。
In Pop III stellar models convection-induced mixing between H- and He-rich burning layers can induce a burst of nuclear energy and thereby substantially alter the subsequent evolution and nucleosynthesis in the first massive stars. We investigate H-He shell and core interactions in 26 stellar evolution simulations with masses $15 - 140\,\mathrm{M}_{\odot}$, using five sets of mixing assumptions. In 22 cases H-He interactions induce local nuclear energy release in the range $ \sim 10^{9} - 10^{13.5}\,\mathrm{L}_{\odot}$. The luminosities on the upper end of this range amount to a substantial fraction of the layer's internal energy over a convective advection timescale, indicating a dynamic stellar response that would violate 1D stellar evolution modelling assumptions. We distinguish four types of H-He interactions depending on the evolutionary phase and convective stability of the He-rich material. H-burning conditions during H-He interactions give $^{12}\mathrm{C}/^{13}\mathrm{C}$ ratios between $\approx 1.5$ to $\sim 1000$ and [C/N] ratios from $\approx -2.3 $ to $\approx 3$ with a correlation that agrees well with observations of CEMP-no stars. We also explore Ca production from hot CNO breakout and find the simulations presented here likely cannot explain the observed Ca abundance in the most Ca-poor CEMP-no star. We describe the evolution leading to H-He interactions, which occur during or shortly after core-contraction phases. Three simulations without a H-He interaction are computed to Fe-core infall and a $140\,\mathrm{M}_{\odot}$ simulation becomes pair-unstable. We also discuss present modelling limitations and the need for 3D hydrodynamic models to fully understand these stellar evolutionary phases.
