γ-ray strength function for astrophysical applications in the IAEA-CRP

¹ Department of Physics, Konan University, Kobe, Japan
² Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, Belgium
³ Department of Physics, University of Oslo, Norway
⁴ Laboratory of Advanced Science and Technology for Industry, University of Hyogo, Japan
⁵ Cyclotron Institute, Texas A & M university, USA
⁶ CEA, DAM, DIF, Arpajon, France
⁷ Nuclear Data Section, International Atomic Energy Agency, Vienna, Austria

^* e-mail: hiro@konan-u.ac.jp

Published online: 30 September 2020

Abstract

The γ-ray strength function (γSF) is a nuclear quantity that governs photoabsorption in (γ, n) and photoemission in (n, γ) reactions. Within the framework of the γ-ray strength function method, we use (γ, n) cross sections as experimental constraints on the γSF from the Hartree-Fock-Bogolyubov plus quasiparticle-random phase approximation based on the Gogny D1M interaction for E1 and M1 components. The experimentally constrained γSF is further supplemented with the zero-limit M1 and E1 strengths to construct the downward γSF with which (n, γ) cross sections are calculated. We investigate (n, γ) cross sections in the context of astrophysical applications over the nickel and barium isotopic chains along the s-process path.