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Csedreki, L. Schiavulli, M. Aliotta, M. Junker, M. Lugaro, M. P. Tak\\'acs, O. Straniero, P. Corvisiero, P. Marigo, P. Prati, R. Depalo, R. Menegazzo, R. Perrino, S. Zavatarelli, T. Chillery, T. Davinson, T. Sz\\\"ucs, V. Mossa, V. Paticchio, Z. Elekes, Zs. F\\\"ul\\\"op","submitted_at":"2022-09-07T10:31:38Z","abstract_excerpt":"In stars, the fusion of $^{22}$Ne and $^4$He may produce either $^{25}$Mg, with the emission of a neutron, or $^{26}$Mg and a $\\gamma$ ray. At high temperature, the ($\\alpha,n$) channel dominates, while at low temperature, it is energetically hampered. The rate of its competitor, the $^{22}$Ne($\\alpha$,$\\gamma$)$^{26}$Mg reaction, and, hence, the minimum temperature for the ($\\alpha,n$) dominance, are controlled by many nuclear resonances. The strengths of these resonances have hitherto been studied only indirectly. 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Best, A. Boeltzig, A. Caciolli, A. Compagnucci, A. Di Leva, A. Formicola, A. Guglielmetti, C. Broggini, C. G. Bruno, C. Gustavino, D. Bemmerer, D. Piatti, D. Rapagnani, E. Masha, E. M. Fiore, F. Barile, F. Cavanna, F. Ferraro, F. R. Pantaleo, G. F. Ciani, G. Gervino, G. Imbriani, Gy. Gy\\\"urky, J. Balibrea-Correa, J. Skowronski, K. St\\\"ockel, L. Csedreki, L. Schiavulli, M. Aliotta, M. Junker, M. Lugaro, M. P. Tak\\'acs, O. Straniero, P. Corvisiero, P. Marigo, P. Prati, R. Depalo, R. Menegazzo, R. Perrino, S. Zavatarelli, T. Chillery, T. Davinson, T. Sz\\\"ucs, V. Mossa, V. Paticchio, Z. Elekes, Zs. F\\\"ul\\\"op","submitted_at":"2022-09-07T10:31:38Z","abstract_excerpt":"In stars, the fusion of $^{22}$Ne and $^4$He may produce either $^{25}$Mg, with the emission of a neutron, or $^{26}$Mg and a $\\gamma$ ray. At high temperature, the ($\\alpha,n$) channel dominates, while at low temperature, it is energetically hampered. 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