The 12C+12C fusion cross-section at sub-coulomb barrier energies

The study of the fusion reaction process of the carbon 12 isotope is not only relevant to get a better understanding of the nucleosynthesis process but also given that it is through this process in which stars obtain their main source of energy.
Measuring the fusion cross-sections of production reactions that form chemical elements is at the centre of interest regarding some astrophysical scenarios. The processes of nucleosynthesis give birth
to heavier elements and, in the carbon scenario, can develop into supernovae type IA explosions or superbursts from accreting neutron stars. In particular, given the significance of carbon to life in general, the reaction 12C+12C is vitally important to understand and has therefore long been studied. However, previous theoretical and experimental efforts show considerable discrepancies as the energy approaches that of the Coulomb barrier, resulting in differing values obtained for the astrophysical S factor. Particularly at low energies, these discrepancies lead to vastly differing hypotheses to describe this phenomenon.
In this work, a direct measurement of the 12C+12C fusion reaction cross-section is performed via coincidences from the evaporated charged particles and the gamma particles produced from the deexcitation of the daughter nucleus, using the STELLA (STELar LAboratory) at IPN (Institut de Physique Nucléaire), Orsay, France.