http://arxiv.org/abs/2111.14980
The $(n,\alpha)$ reaction contributes in many processes of energy generation and nucleosynthesis in stellar environment. Since experimental data are available for a limited number of nuclei and in restricted energy ranges, at present only theoretical studies can provide predictions for all astrophysically relevant $(n,\alpha)$ reaction cross sections. The purpose of this work is to study $(n,\alpha)$ reaction cross sections for a set of nuclei contributing in the s-process nucleosynthesis. Theory framework is based on the statistical Hauser-Feshbach model implemented in TALYS code and supplemented with nuclear properties based on Skyrme energy density functional. In addition to the analysis of the properties of calculated $(n,\alpha)$ cross sections, the Mawellian averaged cross sections are described and analyzed for the range of temperatures in stellar environment. Model calculations determined astrophysically relevant energy windows in which $(n,\alpha)$ reactions occur in massive stars. In order to reduce the uncertainties in modeling $(n,\alpha)$ reaction cross sections for the s-process, novel experimental studies are called for. The results on the predicted relevant $(n,\alpha)$ reaction energy windows for the s-process nuclei provide a guidance for the priority energy ranges for the future experimental studies.
S. Küçüksucu, M. Yiğit and N. Paar
Wed, 1 Dec 21
59/110
Comments: 25 pages, 9 figures