Fusion dynamics of astrophysical reactions using different transmission coefficients

• Main Authors: Rana, Shilpa, Kumar, Raj, Patra, S. K., Bhuyan, Mrutunjaya
• Format: Article
• Published: Springer 2022
• Subjects: QC Physics
• Online Access: http://eprints.um.edu.my/40247/

The heavy-ion fusion reactions play a pivotal role in stellar burning processes in different astrophysical scenarios. The C-12+C-12, C-12+O-16 and O-16+O-16 fusion reactions hold paramount significance in the later stages of the evolution of the heavy mass stars. The stellar energies at which these reactions proceed in astrophysical environments lie far below their respective Coulomb barriers and are beyond the reach of the present experimental laboratories, thus essential to explore the theoretical predictions. In this study, we have investigated the fusion dynamics of astrophysical heavy-ion reactions using the nuclear potential obtained within the relativistic mean-field (RMF) approach. Three different methods, namely the Hill-Wheeler, Ahmed, and Kemble approximations, are used to determine the barrier transmission coefficient at energies of astrophysical significance. The fusion cross-section and the astrophysical S-factor are calculated using the l-summed Wong model. Comparison of the cross-section for all three transmission coefficients with the experimental data manifested that the Kemble approximation gives a better overlap with the experimental data at far below barrier energies. Thus, the Kemble transmission coefficient furnished with nuclear potential obtained from RMF formalism is observed to be suitable for determining the reaction rates of fusion reactions at energies of astrophysical significance.