https://doi.org/10.1140/epja/s10050-023-00957-1
Letter
Direct measurement of the 
F(p,
)
O reaction at E
= 0.4–0.9 MeV using the LHASA detector array
1
Laboratori Nazionali del Sud INFN, Catania, Italy
2
Extreme Light Infrastructure Nuclear Physics/IFIN-HH, Magurele, Romania
3
Scoala Doctorala de Ingineria si Aplicatiile Laserilor si Acceleratorilor, Universitatea Politehnica, Bucharest, Romania
4
Università di Enna “Kore”, Enna, Italy
5
Instituto de Física, Universidad Nacional Autónoma de México, Mexico City, Mexico
6
Dipartimento di Fisica e Astronomia “E. Majorana”, Università degli Studi di Catania, Catania, Italy
7
Nuclear Physics Institute of ASCR, Rez, Czech Republic
8
Dipartimento di Fisica, Università di Napoli Federico II, Naples, Italy
9
Centro Siciliano di Fisica Nucleare e Struttura della Materia (CSFNSM), Catania, Italy
10
Dipartimento di Fisica e Geologia, Università di Perugia, Perugia, Italy
11
INFN-Sezione di Perugia, Perugia, Italy
12
Instituto de Estructura de la Materia, Consejo Superior de Investigaciones Científicas, Madrid, Spain
Received:
27
October
2022
Accepted:
19
February
2023
Published online:
31
March
2023
The F(p,
)O reaction is of paramount importance for understanding the fluorine abundance in the outer layers of asymptotic giant branch (AGB) stars and it might also play a role in hydrogen-deficient post-AGB star nucleosynthesis. Theoretical models overestimate F abundances in AGB stars with respect to the observed values, thus calling for further investigation of the reactions involved in the fluorine nucleosynthesis. In the last years, new direct and indirect measurements improved significantly the knowledge of the F(p,)O cross section at deeply sub-Coulomb energies (below 0.8 MeV). Those data are larger by a factor of about 1.4 with respect to the previous data reported in the NACRE compilation in the energy region 0.6–0.8 MeV. In order to solve these discrepancies, here we present a new direct experiment performed using a silicon strip detector array (LHASA – Large High-resolution Array of Silicon for Astrophysics). Our results clearly confirm the trend of the latest experimental data in the energy region of interest, pointing towards a larger S-factor value than the one reported in the NACRE compilation.
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© The Author(s), under exclusive licence to Società Italiana di Fisica and Springer-Verlag GmbH Germany, part of Springer Nature 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law.
