A technique for the study of (n,p) reactions of astrophysical interest with SECAR

Neutron-induced reactions are essential for the advancement of nucleosynthesis for elements heavier than iron. Recent studies show that key (n,p) reactions starting from $^{56}$Ni accelerate the so-called neutrino-p process, enabling the synthesis of heavy elements in type II Supernovae. The $\nu$p-process occurs in slightly proton-rich regions in the neutrino-driven wind of core-collapse supernovae, via a sequence of (p,$\gamma$) and (n,p) reactions, where a small abundance of neutrons originates from anti-neutrino captures on free protons. The study of such (n,p) reactions is achievable via the measurement of the reverse (p,n) reactions. The challenge in studying such reactions is that the recoils and the unreacted projectiles have nearly identical masses. An appropriate separation level is achievable with the SEparator for CApture Reactions at FRIB. The first direct measurement of the p($^{58}$Fe,n)$^{58}$Co reaction was possible by the in-coincidence detection of the $^{58}$Co at the end of SECAR and the emitted neutrons. With this reaction measurement, we pave the path for (p,n) reaction studies of significant astrophysical interest with SECAR using radioactive beams provided by FRIB. In this talk, preliminary results of the aforementioned measurement along with the development of the experimental method will be discussed.