Speaker
Sebastiana Maria Puglia
(LNS)
Description
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{\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy}
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\TITLE{Study of the $^{10}$B(p; $\alpha$)$^{7}$Be reaction at astrophysical energy using the Trojan Horse Method
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\AUTHORS{S.M.R. Puglia$^{1}$, C. Spitaleri$^{1,2}$, M. La Cognata$^{1}$, L. Lamia$^{2}$, C. Broggini$^{3}$, A. Caciolli $^{3,4}$, N. Carlin $^{5}$, S. Cherubini $^{1,2}$, A. Cvetinovic $^{1}$ , D. Dell'Aquila $^{6,7}$, R. Depalo $^{3,4}$, M. Gulino $^{1,8}$, I. Lombardo $^{6,7}$, R. Menegazzo $^{3}$, M.G. Munhoz$^{5}$, R.G. Pizzone$^{1}$, G.G. Rapisarda $^{1,2}$, V. Rigato$^{9}$, S. Romano$^{1,2}$, M.L. Sergi $^{1}$, F.A. Souza $^{5}$, R. Spart\'a $^{1}$, A. Tumino$^{1,8}$}
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\AFFILIATION{1}{INFN-Laboratori Nazionali del Sud, Catania, Italy}
\AFFILIATION{2}{Dipartimento di Fisica e Astronomia, University of Catania, Catania, Italy}
\AFFILIATION{3}{INFN-Padova, Padova, Italy}
\AFFILIATION{4}{Dipartimento di Fisica, University of Padova, Padova, Italy}
\AFFILIATION{5}{Departamento de Fisica Nuclear, Universitade de Sao Paulo, Brasil }
\AFFILIATION{6}{Dipartimento di Fisica, University of Napoli, Napoli, Italy}
\AFFILIATION{7}{INFN-Napoli, Napoli , Italy}
\AFFILIATION{8}{Facolt\'a di Ingegneria e Architettura," Kore" University, Enna, Italy}
\AFFILIATION{9}{INFN-Laboratori Nazionali di Legnaro, Legnaro, Italy}
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\centerline{Contact email: {\it puglia@lns.infn.it}}
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The study of the reactions involving boron is of particular importance in nuclear physics as well as in nuclear astrophysics. In nuclear physics, it is possible to investigate the $^{11}$C level that are presently poorly known. On the nuclear astrophysics side the reactions destroying boron are important for understanding the abundances of light elements in stellar interior; in particular $^{10}$B(p,$\alpha$)$^{7}$Be reaction is the main responsible for $^{10}$B destruction in stars [1]. In such environments this p-capture process occurs at a Gamow energy of 10 keV, and takes places mainly through a resonant state (E$_{x}$=8.701 MeV) of the compound $^{11}$C 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 $^{10}$B(p, $\alpha$)$^{7}$Be reaction was studied via the THM applied to the $^{2}$H($^{10}$B,$\alpha$$^{7}$Be)n in order to extract the astrophysical S(E)-factor in a wide energy range, from 5 keV to 1.5 MeV.\\ Two set of data will be presented , one of the experiment at LNS in Catania [2] and the other one was performed at Pelletron Linac Laboratory (Departamento de Fisica Nuclear DFN) in Sao Paolo (Brazil), respectively at 24.5 MeV and 27 MeV $^{10}$B energy [3] .
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\noindent [1] A.M. Boesgaard et al., Astrophys. Journ. 621, 991 (2005);
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[2] C. Spitaleri et al., Phys-ReV. C 90, 035801 (2014);
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[3] C. Spitaleri et al., Phys-ReV. C in press, (2017).}
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Primary author
Sebastiana Maria Puglia
(LNS)
