Measurement of neutron capture cross sections of copper from 1 eV to 700 keV at CSNS Back-n*

作者：Yubing Li, 安振东, Wei Jiang, Ma Yx, Cheng Li, Jie Ren, xichao ruan, Jingyu Tang, Rui-Rui Fan, Di Sun, Li Liu, Jingyi Zhang, Ruoran Bai, Shaokun Liu, Chenchen Guo, Hao Liang, Junheng Hu, Ting Liu, H W Wang, Yi Sui, Xian-Kai Li, X X Li, Wen 罗文 Luo, Yaju Chen, Wen Xie, Zhouji Liao, Hu Xin-Rong, Chun-Wang 马春旺 Ma, Han Yi, Yuehua Chen, Qi Li, Zhixin Tan, Hantao Jing · 发表于：Chinese Physics C · 年份：2026 · DOI：10.1088/1674-1137/ae71a5 · 被引用次数：2 · 研究领域：Radiation Therapy and Dosimetry、Nuclear reactor physics and engineering、Radioactive Decay and Measurement Techniques

Abstract The neutron capture cross sections of copper play a crucial role in the s process of stellar nucleosynthesis, the production of the medical isotope 64 Cu for PET imaging and radiotherapy, and Neutron Resonance Capture Analysis for determining the elemental and isotopic compositions of archaeological and cultural heritage materials. The Cu(n,γ) cross section was measured from 1 eV to 700 keV at the Back-n facility of the Chinese Spallation Neutron Source using the time-of-flight method. Prompt γ-rays were detected by four C 6 D 6 liquid scintillator detectors, and the data were analyzed using the pulse height weighting technique. The results are generally consistent with the evaluated data in the major library; however, some discrepancies were observed, offering valuable insights into the differences between five prominent evaluated data libraries. The R -matrix SAMMY code was used to extract the resonance parameters for 63,65 Cu in the resolved resonance region. Maxwellian-averaged cross sections were calculated within the temperature range relevant to the s process nucleosynthesis model, spanning kT =5-100 keV, based on the averaged cross sections in the unresolved resonance region. At kT =30 keV, the MACSs values for 63 Cu (88.1±8.8 mb) and 65 Cu (42.1±4.2 mb) were higher than the corresponding recommendations in the Karlsruhe Astrophysical Database of Nucleosynthesis in Stars.