发表机构
School of Physics, Anhui University; Institute of Radiation Technology, Beijing Academy of Science and Technology; Department of Nuclear Physics, China Institute of Atomic Energy（安徽大学物理学院; 北京市科学技术研究院辐射技术研究所; 中国原子能科学研究院核物理系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用特洛伊木马方法，以氮-14为核，通过准自由反应测量碳-12+碳-12聚变反应，提取天体物理S*(E)因子，发现其随能量降低而上升，为恒星演化与超新星研究提供参考。
AI 中文摘要
$^{12}$C+$^{12}$C 聚变反应是恒星演化和超新星爆炸中的关键物理过程。它不仅决定了质量恒星晚期的演化命运，还直接影响吸积白矮星中触发 Ia 型超新星的关键条件。在本工作中，采用 THM（ Trojan Horse Method，特洛伊木马方法）研究 $^{12}$C+$^{12}$C 聚变过程中 $^{12}$C($^{12}$C,α0)$^{20}$Ne 反应道，以 $^{14}$N 作为特洛伊木马核。望远镜探测器分别放置在 0° 和 15° 位置，设计了两种实验构型，覆盖旁观者粒子最可能出现的向前角区域。通过应用 DWBA（扭曲波玻恩近似），从三体反应 $^{12}$C($^{14}$N,dα0)$^{20}$Ne 中提取了两组二体反应 $^{12}$C($^{12}$C,α0)$^{20}$Ne 的天体物理 S*(E) 因子，并将其归一化到现有实验数据。结果表明，受限于整体实验分辨率，本研究无法分辨精细共振结构。在天体物理能量区域 0.5-2 MeV 内，提取的 S*(E) 因子向低能方向呈上升趋势。0° 构型获得的 S*(E) 因子比 15° 构型获得的趋势更平坦。在准自由反应模拟结果的支持下，两组数据之间的差异可能反映了实验接收度效应、有限探测器分辨率以及反应机制相对贡献可能差异的综合作用。本研究对实验设计、准自由事件选择策略和潜在物理机制的解释进行了系统考察，为理解 $^{12}$C+$^{12}$C 聚变反应在天体物理过程中的作用提供了有益参考。
英文摘要
The 12C+12C fusion reaction is a key physical process in stellar evolution and supernova explosions. It not only determines the late evolutionary fate of massive stars but also directly influences the critical conditions for triggering Type Ia supernovae in accreting white dwarfs. In this work, the THM was employed to investigate the 12C(12C,a0)20Ne reaction channel of the 12C+12C fusion process, using 14N as the Trojan horse nucleus. Telescope detectors were placed at 0 and 15 deg. to design two experimental configurations covering the forward-angle regions where spectator particles are most likely to emerge. By applying the DWBA, two sets of astrophysical S*(E) factors for the two-body reaction 12C(12C,a0)20Ne were extracted from the three-body reaction 12C(14N,da0)20Ne and normalized to existing experimental data. The results show that, limited by the overall experimental resolution, the present study cannot resolve fine resonance structures. Within the astrophysical energy region of 0.5-2 MeV, the extracted S*(E) factor exhibits an increasing trend toward lower energies. The S*(E) factor obtained with the 0-deg configuration shows a flatter trend than that obtained with the 15-deg configuration. Supported by the quasi-free reaction simulation results, the divergence between the two data sets may reflect a combination of experimental acceptance effects, finite detector resolution, and possible differences in the relative contributions of reaction mechanisms. This study provides a systematic examination of the experimental design, quasi-free event selection strategy, and interpretation of the underlying physical mechanisms, serving as a useful reference for understanding the role of the 12C+12C fusion reaction in astrophysical processes.
CommentsIt is to be published in Chinese Physics C
