发表机构
University of Surrey; University of Notre Dame; Universidad Nacional Autónoma de México; University of Birmingham（萨里大学; 圣母大学; 墨西哥国立自治大学; 伯明翰大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究首次直接测量了$^{45}$Sc($p,γ$)$^{46}$Ti反应在526–1275 keV能量范围内的六个低能共振强度，更新了热核反应速率，对理解大质量恒星及新星中的核合成具有重要意义。
AI 中文摘要
$^{45}$Sc($p,\gamma$)$^{46}$Ti 反应在静水燃烧和爆炸性核合成过程中均扮演重要角色。在大质量恒星的静水氧燃烧和硅燃烧阶段，包括对流碳氧（C-O）壳层合并等动态过程，该反应作为瓶颈，调控着Sc-Ti质量区域的反应流。在氧氖（ONe）新星中，喷出物表明产生了直至铁族的元素，如V1974 Cygni中所观测到的，而$^{45}$Sc($p,\gamma$)$^{46}$Ti 反应将钙以上的核素与铁区域联系起来。在核心坍缩超新星（CCSNe）中，该反应影响放射性同位素$^{47}$Sc的产生。目前，热核反应速率基于统计模型计算。本工作中，我们报告了利用圣母大学核科学实验室5 MV加速器，在实验室质子能量范围526–1275 keV内对$^{45}$Sc($p,\gamma$)$^{46}$Ti反应进行的测量。我们首次直接测量了六个共振的共振强度，其共振能量分别为$E^{\rm lab}_{\rm R}$ = 917.4、1026.0、1031.1、1049.7、1059.4和1257.5 keV，并给出了在$E^{\rm lab}$ = 555、630、700、761和871 keV处的积分共振强度。对于低于最低直接测量能量的共振，我们利用现有的转移反应数据来估算共振强度。我们推导了更新的热核反应速率，并讨论了其天体物理意义。
英文摘要
The $^{45}$Sc($p,γ$)$^{46}$Ti reaction plays an important role in both hydrostatic and explosive nucleosynthesis. During hydrostatic oxygen and silicon burning in massive stars, including dynamic processes such as convective carbon-oxygen (C-O) shell mergers, it acts as a bottleneck that regulates the reaction flow in the Sc-Ti mass region. In oxygen-neon (ONe) novae, the ejecta indicate the production of elements up to the Fe group, as observed in V1974 Cygni, and the $^{45}$Sc($p,γ$)$^{46}$Ti reaction links nuclei above Ca to the Fe region. In core-collapse supernovae (CCSNe), it influences the production of the radioactive isotope $^{47}$Sc. At present, the thermonuclear reaction rate is based on statistical model calculations. In this work, we report on measurements of the $^{45}$Sc($p,γ$)$^{46}$Ti reaction performed using the 5~MV accelerator at the Nuclear Science Laboratory, University of Notre Dame, over a laboratory proton energy range of 526--1275~keV. We present the first direct measurements of the resonance strengths for six resonances at $E^{\rm lab}_{\rm R} = 917.4$, 1026.0, 1031.1, 1049.7, 1059.4 and 1257.5~keV, together with integrated resonance strengths at $E^{\rm lab} = 555$, 630, 700, 761 and 871~keV. For resonance energies below the lowest directly measured energy, available transfer-reaction data were used to estimate the resonance strengths. An updated thermonuclear reaction rate is derived, and its astrophysical implications are discussed.
Journal refR. S. Sidhu et al., Physical Review C 114, 035807 (2026)
