Speaker
Description
The radioisotope ${}^{26}\mathrm{Al}$ plays a crucial role in understanding the origins of cosmic elements, particularly at active nucleosynthesis sites such as supernovae and massive star-forming regions. Its characteristic $1809\,\mathrm{keV}$ $\gamma$-ray emission, observed by gamma telescopes, serves as direct evidence of ongoing nucleosynthesis processes. Neutron-induced reactions, specifically the ${}^{26}\mathrm{Al}(n,p)$ and ${}^{26}\mathrm{Al}(n,\alpha)$ reactions, have been identified as key contributors to the ${}^{26}\mathrm{Al}$ abundance in core-collapse supernova ejecta.
Despite recent progress in measuring these reaction rates up to temperatures of $\sim 1\,\mathrm{GK}$, which are relevant to some ${}^{26}\mathrm{Al}$ creation sites, it remains insufficient for explosive scenarios occurring at temperatures between 1.5 and $3.5\,\mathrm{GK}$. Experimental data for these temperatures are currently lacking due to several challenges. These include the necessity for a powerful neutron source at the relevant energies, constraints on radioactive sample size, and difficulty measuring outgoing charged particles in high radiation environments.
In this study, we propose a novel experimental approach using the ${}^{7}\mathrm{Li}(p,n)$ reaction to generate broad-energy neutron beams. Coupled with a gaseous Micromegas detector, this setup will enable comprehensive measurement of ${}^{26}\mathrm{Al}(n,p)$ and ${}^{26}\mathrm{Al}(n,\alpha)$ reaction rates across the relevant energy range. Our study aims to advance cosmic nucleosynthesis understanding and enhance astrophysical modeling by bridging this knowledge gap.
