在CSNS Back-n中测量[公式:见文本]Ta([公式:见文本]) 截面到恒星 s 过程温度
Zhendong An1,2,3,4,5, Weiwei Qiu2,3,4, Wei Jiang6,7
1School of Physics and Astronomy, Sun Yat-sen University, Zhuhai, 519082 China.
Scientific reports
|August 4, 2023
概括
对-181中子捕获截面的新测量为核天体物理学和能源系统提供了关键数据. 这项研究揭示了在恒星温度下麦克斯韦平均截面的差异,影响了核合成模型.
科学领域:
- 核天体物理学 核天体物理学
- 核能是核能中的一种.
- 行星地质学 行星地质学
背景情况:
- -181 (181Ta) 的中子捕获截面对于理解恒星核合成 (s过程) 是至关重要的.
- 准确的截面数据对于设计先进的核能系统和分析外星样本至关重要.
研究的目的:
- 精确测量181Ta (n, γ) 截面在广泛的能量范围内.
- 通过确定麦克斯韦平均截面 (MACS) 来完善天体物理计算.
- 将实验结果与现有的核数据库和理论模型进行比较.
主要方法:
- 使用了中国支离子中子源 (CSNS) 的背流白中子设施 (Back-n).
- 采用了飞行时间 (TOF) 技术,使用了181个液体闪探测器来检测中子.
- 应用R-矩阵分析使用SAMMY代码提取从1 eV到700 eV的共振参数.
主要成果:
- 测量了从1 eV到800 keV的181Ta (n, γ) 截面.
- 在已解决和未解决的共振区域中提取了共振参数.
- 对于恒星温度 (kT = 5100 keV) 的计算MACS,在kT = 30 keV时产生834 ± 75 mb.
- 观察到与KADoNiS推值 (766 ± 15 mb) 有显著差异.
结论:
- 新的181Ta (n, γ) 截面测量为恒星环境中的s过程提供了更强大的约束.
- 发现的MACS差异凸显了在天体物理模型中重新评估核数据的必要性.
- 这些发现有助于改善核天体物理学理解和核能潜在应用.
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