论文标题
$ {^{^{44}} $ ti和$ {^{56}} $ ni生产的敏感性
Sensitivity of ${^{44}}$Ti and ${^{56}}$Ni production in CCSN shock-driven nucleosynthesis to reaction rates
论文作者
论文摘要
最近的观察性进步已启用了$ {^{44}} $ ti的高分辨率映射，以核心折叠超新星（CCSN）残留物。观测和模型之间的比较对CCSN机制提供了严格的约束。但是，过去的工作已经确定了几个不确定的核反应率，这些核反应率会影响$ {^{44}} $ ti和$ {^{56}} $ ni在后处理模型计算中产生。我们进化了一维模型，$ 15〜m _ {\ odot} $，$ 18〜m _ {\ odot} $，$ 22〜m _ {\ odot} $和$ 25〜m _ {\ odot} $ a {\ odot} $ a} $ sarts in ccsn a r {研究了$ {^{44}} $ ti和$ {^{56}} $ ni生产的先前确定的反应速率灵敏度。我们通过对CCSN爆炸能量和质量量的各种假设进行了各种假设来测试结果的鲁棒性。我们发现许多反应对$ {^{44}} $ ti和$ {^{56}} $ ni的核合成有重大影响，尤其是对于较低的祖细胞质量。值得注意的是，反应率$^{13} {\ rm n}（α，p）^{16} {\ rm o} $，$^{17} {\ rm f}（\ rm f}（α，p）^{20} {\ rm ne} {\ rm ne} fe}（α，p）^{55} {\ rm co} $，$^{56} {\ rm ni} {\ rm ni}（α，p）^{59} {\ rm cu} $，$^，$^{57} {57} {\ rm ni} {\ rm ni} { $^{56} {\ rm co}（p，n）^{56} {\ rm ni} $，$^{39} {\ rm k}（\ rm k}（p，γ）^{40} {\ rm ca} {\ rm ca} cr} $，$^{52} {\ rm mn}（p，γ）^{53} {\ rm fe} $，$^{57} {\ rm co}（p，γ） k}（p，α）^{36} {\ rm ar} $对大量模型条件有影响。此外，我们发现通过先前对CCSN休克驱动的核合成的后处理研究确定的有影响力反应的列表可能是不完整的，这激发了未来的较大规模的灵敏度研究。
Recent observational advances have enabled high resolution mapping of ${^{44}}$Ti in core-collapse supernova (CCSN) remnants. Comparisons between observations and models provide stringent constraints on the CCSN mechanism. However, past work has identified several uncertain nuclear reaction rates that influence ${^{44}}$Ti and ${^{56}}$Ni production in post-processing model calculations. We evolved one dimensional models of $15~M_{\odot}$, $18~M_{\odot}$, $22~M_{\odot}$ and $25~M_{\odot}$ stars from zero-age main sequence through CCSN using {\tt MESA} (Modules for Experiments in Stellar Astrophysics) and investigated the previously identified reaction rate sensitivities of ${^{44}}$Ti and ${^{56}}$Ni production. We tested the robustness of our results by making various assumptions about the CCSN explosion energy and mass-cut. We found a number of reactions that have a significant impact on the nucleosynthesis of ${^{44}}$Ti and ${^{56}}$Ni, particularly for lower progenitor masses. Notably, the reaction rates $^{13}{\rm N}(α,p)^{16}{\rm O}$, $^{17}{\rm F}(α,p)^{20}{\rm Ne}$, $^{52}{\rm Fe}(α,p)^{55}{\rm Co}$, $^{56}{\rm Ni}(α,p)^{59}{\rm Cu}$, $^{57}{\rm Ni}(n,p)^{57}{\rm Co}$, $^{56}{\rm Co}(p,n)^{56}{\rm Ni}$, $^{39}{\rm K}(p,γ)^{40}{\rm Ca}$, $^{47}{\rm V}(p,γ)^{48}{\rm Cr}$, $^{52}{\rm Mn}(p,γ)^{53}{\rm Fe}$, $^{57}{\rm Co}(p,γ)^{58}{\rm Ni}$, and $^{39}{\rm K}(p,α)^{36}{\rm Ar}$ are influential for a large number of model conditions. Furthermore, we found the list of influential reactions identified by previous post-processing studies of CCSN shock-driven nucleosynthesis is likely incomplete, motivating future larger-scale sensitivity studies.
