Fusion of 12C + 24Mg at extreme sub-barrier energies. (1st September 2022)

• Record Type: Journal Article
• Authors: Montagnoli, G; Stefanini, A M; Jiang, C L; Hagino, K; Niola, F; Brugnara, D; Čolović, P; Colucci, G; Corradi, L; Depalo, R; Fioretto, E; Goasduff, A; Pasqualato, G; Scarlassara, F; Szilner, S; Zanon, I
• Is Part Of: Journal of physics. Volume 49:Number 9(2022)
• Publication Date: 2022-09-01
• Subjects: heavy-ion fusion -- sub-barrier cross sections -- coupled-channels model -- electrostatic beam deflector; Nuclear physics -- Periodicals; Particles (Nuclear physics) -- Periodicals; Physique nucléaire -- Périodiques; Particules (Physique nucléaire) -- Périodiques; Kernfysica; Elementaire deeltjes; 539.7
• DOI: 10.1088/1361-6471/ac7edd
• Languages: English
• ISSNs: 0954-3899

Abstract

Abstract: A recent experiment on 12 C + 24 Mg sub-barrier fusion was performed. Standard coupled-channels calculations clearly over-estimated the low energy cross sections and there was indication of a maximum of the astrophysical S factor vs energy. In the present work further measurements have been performed on the same system, and we extended the excitation function to lower energies down to σ ≃ 4 μ b, confirming the existence of the hindrance phenomenon. Additional energy points near the barrier were added as well. In agreement with the result of previous experiment, the hindrance energy threshold is observed to correspond to a remarkably large cross section. The present new data allow to better define the S -factor maximum, that is well fitted using two parametrizations of either the hindrance or the adiabatic model. We also performed coupled-channels calculations using a Woods–Saxon potential. Far below the barrier we observe that the coupling strengths decrease and tend to vanish, indeed one-dimensional tunnelling calculations well reproduce the excitation function. Further precise cross section measurements at slightly lower energies are needed to discriminate between the adiabatic and hindrance models. This would give a reliable guidance for the extrapolation to the systems of astrophysical interest, like 12 C + 12 C and 16 O + 16 O.