Microscopic potential model analysis of the radiative $(n,\gamma)$ cross sections near the $Z=50$ shell closure taking part in the main s-component

TL;DR

This paper models neutron capture cross sections near the Z=50 shell closure using a microscopic potential approach, providing data relevant for astrophysical nucleosynthesis processes.

Contribution

It introduces a microscopic optical potential based on RMF and M3y interactions for calculating neutron capture cross sections near Z=50, enhancing theoretical predictions.

Findings

Calculated Maxwellian-averaged cross sections (MACS) for relevant nuclei.

Provided stellar neutron capture reaction rates at astrophysical energies.

Demonstrated the effectiveness of the microscopic potential model.

Abstract

The neutron capture cross sections have been studied near the $Z=50$ closed shell for a number of nuclei those take part in heavy element nucleosynthesis, the slow and the rapid neutron capture processes and the proton capture process. An optical model potential is constructed in theoretical approach by folding the density dependent M3y purely real nucleon-nucleon interaction with the target radial matter density in relativistic mean field (RMF) approach. The standard code TALYS1.8 is used for cross-section calculation. We have presented the Maxwellian-averaged capture cross-section (MACS) values and stellar neutron capture reaction rates at astrophysically relevant thermal energies and temperatures.