Measurement of the [Formula: see text]Ta([Formula: see text]) cross sections up to stellar s-process temperatures at the CSNS Back-n

The neutron capture cross section of [Formula: see text]Ta is relevant to s-process of nuclear astrophysics, extraterrestrial samples analysis in planetary geology and new generation nuclear energy system design. The [Formula: see text]Ta([Formula: see text]) cross section had been measured between...

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Published in:Scientific reports 2023-08, Vol.13 (1), p.12657-12657, Article 12657
Main Authors: An, Zhendong, Qiu, Weiwei, Jiang, Wei, Yang, Gaole, Li, Xiankai, Liao, Zhengfa, Zhuang, Ziyue, Zhang, Xiaoping, Chen, Shengli, Guo, Chenchen, Xiao, Erxi, Fang, Xiao, Li, Xinxiang, Wang, Hongwei, Hu, Xinrong, Jiang, Bing, Shen, Wenqing, Wang, Jincheng, Ren, Jie, Ruan, Xichao, Wang, Dexin, Zhang, Su-Yalatu, Luo, Wen, Zhu, Zhichao, Lan, Haoyang, Cao, Zongwei, Ma, Xu, Liu, Yingdu, Wang, Pusen, Yang, Yi, Su, Ping, Deng, Xiangai, He, Wanbing, Ma, Yugang, Ma, Chunwang, Wang, Yuting, He, Pengqin, Tang, Renguang, Zhou, Tao, Wang, Jing, Yi, Han, Zhang, Yue, Chen, Yonghao, Fan, Ruirui, Gao, Keqing, Li, Qiang, Sun, Kang, Tan, Zhixin, Gu, Minhao, Jing, Hantao, Tang, Jingyu
Format: Article
Language:English
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Summary:The neutron capture cross section of [Formula: see text]Ta is relevant to s-process of nuclear astrophysics, extraterrestrial samples analysis in planetary geology and new generation nuclear energy system design. The [Formula: see text]Ta([Formula: see text]) cross section had been measured between 1 eV and 800 keV at the back-streaming white neutron facility (Back-n) of China spallation neutron source(CSNS) using the time-of-flight (TOF) technique and [Formula: see text] liquid scintillator detectors. The experimental results are compared with the data of several evaluated libraries and previous experiments in the resolved and unresolved resonance region. Resonance parameters are extracted using the R-Matrix code SAMMY in the 1-700 eV region. The astrophysical Maxwell average cross section(MACS) from kT = 5 to 100 keV is calculated over a sufficiently wide range of neutron energies. For the characteristic thermal energy of an astrophysical site, at kT = 30keV the MACS value of [Formula: see text]Ta is 834 ± 75 mb, which shows an obvious discrepancy with the Karlsruhe Astrophysical Database of Nucleosynthesis in Stars (KADoNiS) recommended value 766 ± 15 mb. The new measurements strongly constrain the MACS of [Formula: see text]Ta([Formula: see text]) reaction in the stellar s-process temperatures.
ISSN:2045-2322
2045-2322
DOI:10.1038/s41598-023-39603-7