The cross section calculation of 112Sn(α,γ)116Te reaction with different nuclear models at the astrophysical energy range  

作　　者：C. Yalcin 

机构地区：[1]Department of Physics, Kocaeli University, 41380 UmuttepeKocaeli, Turkey

出　　处：《Nuclear Science and Techniques》2017年第8期103-109,共7页核技术（英文）

摘　　要：The theoretical cross section calculations for the astrophysical p process are needed because most of the related reactions are technically very difficult to be measured in the laboratory. Even if the reaction was measured,most of the measured reactions have been carried out at the higher energy range from the astrophysical energies.Therefore, almost all cross sections needed for p process simulation have to be theoretically calculated or extrapolated to the astrophysical energies.^(112)Sn(α,γ)^(116)Te is an important reaction for the p process nucleosynthesis. The theoretical cross section of ^(112)Sn(α,γ)^(116)Te reaction was investigated for different global optical model potentials,level density, and strength function models at the astrophysically interested energies. Astrophysical S factors were calculated and compared with experimental data available in the EXFOR database. The calculation with the optical model potential of the dispersive model by Demetriou et al., and the back-shifted Fermi gas level density model and Brink-Axel Lorentzian strength function model best served to reproduce experimental results at an astrophysically relevant energy region. The reaction rates were calculated with these model parameters at the p process temperature and compared with the current version of the reaction rate library Reaclib and Starlib.The theoretical cross section calculations for the astrophysical p process are needed because most of the related reactions are technically very difficult to be mea- sured in the laboratory. Even if the reaction was measured, most of the measured reactions have been carried out at the higher energy range from the astrophysical energies. Therefore, almost all cross sections needed for p process simulation have to be theoretically calculated or extrapo- lated to the astrophysical energies. 112Sn（α,γ）116Te is an important reaction for the p process nucleosynthesis. The theoretical cross section of 112Sn（α,γ）116Te reaction was investigated for different global optical model potentials, level density, and strength function models at the astro- physically interested energies. Astrophysical S factors were calculated and compared with experimental data available in the EXFOR database. The calculation with the optical model potential of the dispersive model by Demetriou et al., and the back-shifted Fermi gas level density model and Brink-Axel Lorentzian strength function model best served to reproduce experimental results at an astrophysi- cally relevant energy region. The reaction rates were cal- culated with these model parameters at the p process temperature and compared with the current version of the reaction rate library Reaclib and Starlib.

关 键 词：核反应模型 天体物理学 截面计算 能量范围 光学模型势 模型参数计算 函数模型 能级密度 

分 类 号：O571.41[理学—粒子物理与原子核物理] P14[理学—物理]