EPJ Web Conf.
Volume 260, 2022The 16th International Symposium on Nuclei in the Cosmos (NIC-XVI)
|Number of page(s)||5|
|Section||Nuclear Reaction Rates and Stellar Abundances|
|Published online||24 February 2022|
Direct measurements of the 12C(12C,p)23Na and 12C(12C,α)20Ne reactions at low energies for Nuclear Astrophysics
1 INFN, Sezione di Napoli, Napoli, Italy
2 SUPA, School of Physics and Astronomy, University of Edinburgh, Edinburgh, UK
3 Dipartimento di Matematica e Fisica, Università degli Studi della Campania “Luigi Vanvitelli”, Caserta, Italy
4 Dipartimento di Fisica “E. Pancini”, Università degli Studi di Napoli “Federico II”, Napoli, Italy
5 Centro Italiano di Ricerche Aerospaziali, Capua, Italy
6 Departamento de Física Nuclear, Instituto de Física da Universidade de São Paulo, São Paulo, Brazil
* e-mail: email@example.com
Published online: 24 February 2022
12C+12C reactions are crucial in the evolution of massive stars and explosive scenarios. The measurement of these reactions at astrophysical energies is very challenging due to their extremely small cross sections, and the presence of beam induced background originated by the natural 1,2H contaminants in the C targets. In addition, the many discrepancies between different data sets and the complicated resonant structure of the cross sections make the extrapolation to low energies very uncertain. Recently, we performed a direct measurement of the 12C+12C reactions at the CIRCE Laboratory in Italy. Results from a study on target contamination were used, allowing us to measure cross sections at Ec.m. =2.51 − 4.36 MeV with 10-25 keV energy steps. Two stage ΔE-Erest detectors were used for unambiguous particle identiﬁcation. Branching ratios of individual particle groups were found to vary signiﬁcantly with energy and angular distributions were also found to be anisotropic, which could be a potential explanation for the discrepancies observed among different data sets.
© The Authors, published by EDP Sciences, 2022
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