Data di Pubblicazione:
2023
Citazione:
Improved S factor of the C12(p,γ)N13 reaction at E=320–620 keV and the 422 keV resonance / J. Skowronski, E. Masha, D. Piatti, M. Aliotta, H. Babu, D. Bemmerer, A. Boeltzig, R. Depalo, A. Caciolli, F. Cavanna, L. Csedreki, Z. Fülöp, G. Imbriani, D. Rapagnani, S. Rümmler, K. Schmidt, R.S. Sidhu, T. Szücs, S. Turkat, A. Yadav. - In: PHYSICAL REVIEW C. - ISSN 2469-9985. - 107:6(2023), pp. L062801.1-L062801.6. [10.1103/PhysRevC.107.L062801]
Abstract:
The ¹²C(p,γ)¹³N reaction is the onset process of both the CNO and hot CNO cycles that drive massive star, red and asymptotic giant branch star, and novae nucleosynthesis. The ¹²C(p,γ)¹³N rate affects the final abundances of the stable ¹²´¹³C nuclides with ramifications for meteoritic carbon isotopic abundances and the s-process neutron source strength. Here, an underground measurement of the ¹²C(p,γ)¹³N cross section is reported. The present data, obtained at the Felsenkeller shallow-underground laboratory in Dresden (Germany), encompass the 320–620 keV center of mass energy range to include the wide and poorly constrained E=422 keV resonance that dominates the rate at high temperatures. This work's S-factor results, lower than literature by 25%, are included in a comprehensive R-matrix fit, and the energy of the 12+ first excited state of ¹³N is found to be 2369.6(4) keV with a radiative and proton width of 0.49(3) eV and 34.9(2) keV, respectively. A reaction rate, based on the present R-matrix fit and extrapolation, is suggested.
Tipologia IRIS:
01 - Articolo su periodico
Elenco autori:
J. Skowronski, E. Masha, D. Piatti, M. Aliotta, H. Babu, D. Bemmerer, A. Boeltzig, R. Depalo, A. Caciolli, F. Cavanna, L. Csedreki, Z. Fülöp, G. Imbriani, D. Rapagnani, S. Rümmler, K. Schmidt, R.S. Sidhu, T. Szücs, S. Turkat, A. Yadav
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