AI 中文总结
研究第III星族和富铁第II星族对不稳定超新星的核合成特征。通过探索第III星族PISNe的演化及核合成，研究反应速率不确定性影响；利用时间相关对流模型研究第II星族PISNe，揭示其独特化学特征，为识别早期宇宙PISN遗迹提供诊断。
AI 中文摘要
最近发现的极贫金属（VMP）恒星LAMOST J1010+2358呈现出一种特殊的丰度模式，与约260 M$_\odot$的第III星族对不稳定超新星（PISN）非常吻合。受此启发，我们研究第III星族和第II星族PISNe的核合成特征，为未来观测提供理论约束。本文分为两部分。首先，探索初始质量为130 - 300 M$_\odot$的第III星族PISNe的演化和核合成，研究$^{12}$C$(\alpha,\gamma)^{16}$O和$^{16}$O+$^{16}$O反应速率不确定性对其爆炸特性和核合成的影响。发现奇数Z元素产量对$^{12}$C$(\alpha,\gamma)^{16}$O速率特别敏感，铁峰元素产量对两种速率都敏感。其次，研究仅由第III星族PISN抛射物富集的气体中形成的第II星族PISNe的核合成特征。通过在爆炸过程中采用时间相关对流模型，证明金属富集增加不透明度并引发剧烈对流混合，显著增强爆炸能量和$^{56}\text{Ni}$产量。第II星族PISNe表现出独特化学特征，包括较弱的奇偶效应和增强的锌 - 锗产量，为识别早期宇宙中的PISN遗迹提供独特诊断。
英文摘要
Recently discovered very metal-poor (VMP) star LAMOST J1010+2358 shows a peculiar abundance pattern that is remarkably well fit by a Pop III pair-instability supernova (PISN) of $\simeq 260$ M$_\odot$. Motivated by this, we investigate the nucleosynthetic characteristics of Pop III and Pop II PISNe to provide theoretical constraints for future observations. This paper is divided into two parts. First, we explore the evolution and nucleosynthesis of Pop III PISNe with initial masses of 130 - 300 M$_\odot$. Our main aim is to investigate how the uncertainty in $^{12}$C$(α,γ)^{16}$O and $^{16}$O+$^{16}$O reaction rates affect their explosion properties and nucleosynthesis. We find that the yields of odd-$Z$ elements are particularly sensitive to the $^{12}$C$(α,γ)^{16}$O rate, while the production of Fe-peak elements shows significant sensitivity to both rates. Second, we investigate the nucleosynthetic features of Pop II PISNe formed in gas enriched exclusively by Pop III PISN ejecta. By employing a time-dependent convection model during the explosion, we demonstrate that metal enrichment increases opacity and triggers vigorous convective mixing. This hydrodynamic effect significantly enhances the explosion energy and $^{56}\text{Ni}$ production. Consequently, Pop II PISNe exhibit distinct chemical signatures, including a weaker odd-even effect and enhanced Zn-Ge production, providing unique diagnostics for identifying PISN remnants in the early Universe.
Comments26 pages, 25 figures
