https://doi.org/10.1140/epja/s10050-022-00893-6
Regular Article - Theoretical Physics
Fusion dynamics of astrophysical reactions using different transmission coefficients
1
School of Physics and Materials Science, Thapar Institute of Engineering and Technology, 147004, Patiala, India
2
Institute of Physics, Sachivalya Marg, 751005, Bhubaneswar, India
3
Training School Complex, Homi Bhabha National Institute, Anushakti Nagar, 400094, Mumbai, India
4
Center for Theoretical and Computational Physics, Department of Physics, Faculty of Science, University of Malaya, 50603, Kuala Lumpur, Malaysia
5
Institute of Research and Development, Duy Tan University, 550000, Da Nang, Vietnam
6
Faculty of Natural Science, Duy Tan University, 550000, Da Nang, Vietnam
Received:
24
June
2022
Accepted:
24
November
2022
Published online:
12
December
2022
The heavy-ion fusion reactions play a pivotal role in stellar burning processes in different astrophysical scenarios. The C+
C,
C+
O and
O+
O 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
-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.
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© The Author(s), under exclusive licence to Società Italiana di Fisica and Springer-Verlag GmbH Germany, part of Springer Nature 2022. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law.