Abstract
Theγ-ray strength function (γSF) is a nuclear quantity that governs photoabsorption in (γ, n) and photoemission in (n, γ) reactions. Within the framework of theγ-ray strength function method, we use (γ, n) cross sections as experimental constraints on theγSF from the Hartree-Fock-Bogolyubov plus quasiparticle-random phase approximation based on the Gogny D1M interaction for E1 and M1 components. The experimentally constrainedγSF is further supplemented with the zero-limitM1 andE1 strengths to construct the downwardγSF 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.
Highlights
Brink-Axel hypothesis AThe version A is the equality of the upward γ-ray strength function (γSF) built on the ground state and excited states
The γ-ray strength function [1,2,3] is a nuclear statistical quantity of describing the nuclear electromagnetic response that is employed in the Hauser-Feshbach (HF) model [4] of the compound nuclear reaction
The γ-ray strength function (γSF) in the de-excitation mode which we refer to as downward γSF is a key quantity in the HF model calculation of radiative neutron capture cross sections
Summary
The version A is the equality of the upward γSF built on the ground state and excited states. The photoabsorption cross section and the photoneutron cross section for GDR were assumed to be of Lorentzian shape. This hypothesis has led to the experimental investigation of nuclear properties of hot nuclei [8, 9], which was triggered by the observation of radiations from GDR built on highly excited states [10]
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