Resonances above the proton threshold inSi26

Abstract

$^{26}\mathrm{Al}$ remains an intriguing target for observational $\ensuremath{\gamma}$-ray astronomy, thanks to its characteristic decay. The $^{25}\mathrm{Al}(p,\ensuremath{\gamma})^{26}\mathrm{Si}$ reaction is the crucial link in a sequence that bypasses the production of the observable $^{26}\mathrm{Al}^{g}$ in favor of the short-lived isomeric state; determining its astrophysical reaction rate across a range of stellar environments has been the focus of many studies. A reanalysis of previous work, utilizing recent improvements in excitation energies and ground state masses, is presented to reduce the ambiguities in the literature and provide focus to future measurements.