The 10B(p,α)7Be reaction is the main responsible for the 10B destruction in stellar interior [1]. In such environments this p-capture process occurs at a Gamow energy of 10 keV and takes places mainly through a resonant state (Ex = 8.701 MeV) of the compound 11C nucleus. Thus a resonance right in the region of the Gamow peak is expected to significantly influence the behavior of the astrophysical S(E)-factor. The 10B(p,α)7Be reaction was studied via the Trojan Horse Method (THM) applied to the 2H(10B,α7Be)n in order to extract the astrophysical S(E)-factor in a wide energy range from 5 keV to 1.5 MeV.

The B-10(p,alpha)Be-7 S(E)-factor from 5 keV to 1.5 MeV using the Trojan Horse Method / S.M.R. Puglia, C. Spitaleri, M. La Cognata, L. Lamia, C. Broggini, A. Caciolli, N. Carlin, S. Cherubini, A. Cvetinovic, G. D'Agata, D. Dell'Aquila, R. Depalo, M. Gulino, G.L. Guardo, I. Indelicato, I. Lombardo, R. Menegazzo, M.G. Munhoz, R.G. Pizzone, G.G. Rapisarda, V. Rigato, S. Romano, M.L. Sergi, F. Souza, R. Sparta, S. Tudisco, A. Tumino - In: Nuclear Physics in Astrophysics VIII (NPA8 2017) / [a cura di] M. La Cognata. - [s.l] : EDP Sciences, 2017. - ISBN 978-2-7598-9030-9. - pp. 1-4 (( Intervento presentato al 8. convegno International Conference on Nuclear Physics in Astrophysics, NPA8 2017 tenutosi a Catania nel 2017 [10.1051/epjconf/201716501042].

The B-10(p,alpha)Be-7 S(E)-factor from 5 keV to 1.5 MeV using the Trojan Horse Method

S. Cherubini;R. Depalo;
2017

Abstract

The 10B(p,α)7Be reaction is the main responsible for the 10B destruction in stellar interior [1]. In such environments this p-capture process occurs at a Gamow energy of 10 keV and takes places mainly through a resonant state (Ex = 8.701 MeV) of the compound 11C nucleus. Thus a resonance right in the region of the Gamow peak is expected to significantly influence the behavior of the astrophysical S(E)-factor. The 10B(p,α)7Be reaction was studied via the Trojan Horse Method (THM) applied to the 2H(10B,α7Be)n in order to extract the astrophysical S(E)-factor in a wide energy range from 5 keV to 1.5 MeV.
Settore FIS/04 - Fisica Nucleare e Subnucleare
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2434/931211
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