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Fusion dynamics of astrophysical reactions using different transmission coefficients

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Abstract

The heavy-ion fusion reactions play a pivotal role in stellar burning processes in different astrophysical scenarios. The \(^{12}\)C+\(^{12}\)C, \(^{12}\)C+\(^{16}\)O and \(^{16}\)O+\(^{16}\)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 \(\ell \)-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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This manuscript has no associated data or the data will not be deposited. [Authors’ comment: Any data that support the findings of this study are included in the manuscript.]

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Acknowledgements

This work has been supported by Board of Research in Nuclear Sciences (BRNS), Sanction No. 58/14/12/2019-BRNS, Science Engineering Research Board (SERB), File No. CRG/2021/001229, FAPESP Project Nos. 2017/05660-0, and FOSTECT Project No. FOSTECT.2019B.04.

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Authors and Affiliations

  1. School of Physics and Materials Science, Thapar Institute of Engineering and Technology, Patiala, 147004, India

    Shilpa Rana & Raj Kumar

  2. Institute of Physics, Sachivalya Marg, Bhubaneswar, 751005, India

    S. K. Patra

  3. Training School Complex, Homi Bhabha National Institute, Anushakti Nagar, Mumbai, 400094, India

    S. K. Patra

  4. Center for Theoretical and Computational Physics, Department of Physics, Faculty of Science, University of Malaya, Kuala Lumpur, 50603, Malaysia

    M. Bhuyan

  5. Institute of Research and Development, Duy Tan University, Da Nang, 550000, Vietnam

    M. Bhuyan

  6. Faculty of Natural Science, Duy Tan University, Da Nang, 550000, Vietnam

    M. Bhuyan

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  1. Shilpa Rana
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Correspondence to M. Bhuyan.

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Communicated by Alexis Diaz-Torres.

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Rana, S., Kumar, R., Patra, S.K. et al. Fusion dynamics of astrophysical reactions using different transmission coefficients. Eur. Phys. J. A 58, 241 (2022). https://doi.org/10.1140/epja/s10050-022-00893-6

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