Speaker
Description
The astrophysical p-process is crucial for the synthesis of proton-rich isotopes (p-nuclei) that cannot be formed via the s-process or r-process. Occurring primarily in supernovae, this process involves photodisintegration reactions like (γ, n), (γ, p) and (γ, α), driven by high-energy gamma photons, (p, γ) reactions are also relevant in this context. Recent experimental advances, including inverse kinematics and activation methods, have provided essential cross-section data, enhancing the accuracy of theoretical model codes such as TALYS, NON-SMOKER, etc.
In this work, the proton capture (p, γ) cross-sections for p-nuclei in the mass range A = 74–108 have been calculated using TALYS. Consistent input models, including the back-shifted Fermi gas model for level density parameters, Goriely’s hybrid (mic-mac) γ-strength function (option V), and local optical model parameters, are used. Adjusting the 'fiso' parameter for isospin corrections significantly improved our results, which match the experimental data, especially near the energy threshold where the (p,n) channel opens.
References
[1] C. Rolfs, Cauldrons in the Cosmos (University of Chicago Press,1988).
[2] S. Mondal et al., IJMP E, Vol. 31, No. 7 (2022) 2250064
[3] A. J. Koning et al., Nuclear reaction program (NRG-report 21297/04.62741/P).
[4] J. Bork et al., Phys. Rev. C, 58(1), 524 (1998).
| Length of presentation requested | Oral presentation: 8 min + 2 min questions (Poster-type talk) |
|---|---|
| Please select a keyword related to your abstract | Nuclear Theory and Experiments |
