First direct measurement of the N13(α,p)O16 reaction relevant for core-collapse supernovae nucleosynthesis

Le résumé fourni par la source

Understanding the explosion mechanism of a core-collapse supernova (CCSN) is important to accurately model CCSN scenarios for different progenitor stars using model-observation comparisons. The uncertainties of various nuclear reaction rates relevant for CCSN scenarios strongly affect the accuracy of these stellar models. Out of these reactions, the $^{13}\mathrm{N}(\ensuremath{\alpha},p)^{16}\mathrm{O}$ reaction has been found to affect various stages of a CCSN at varying temperatures. This work presents the first direct measurement of the $^{13}\mathrm{N}(\ensuremath{\alpha},p)^{16}\mathrm{O}$ reaction performed using a 34.6 MeV beam of radioactive $^{13}\mathrm{N}$ ions and the active-target detector MUSIC (MUlti-Sampling Ionization Chamber) at Argonne National Laboratory. The resulting total $^{13}\mathrm{N}(\ensuremath{\alpha},p)^{16}\mathrm{O}$ reaction cross sections from this measurement in the center-of-mass energy range of 3.26--6.02 MeV are presented and compared with calculations using the Hauser-Feshbach formalism. Uncertainties in the reaction rate have been dramatically reduced at CCSN temperatures.

Ce résumé expose les affirmations des auteurs. BNTIC ne l’interprète pas comme une validation indépendante des résultats.