Uncertainties in production of stellar 26Al

While most of $^{26}$Al content is believed to be produced in supernovae, as much as 20{\%} may come from novae whose favorable energies enable the precise study of the production mechanism of $^{26}$Al in novae. This study achieves greater importance because $^{26}$Al is one of the critical isotopes that governs the path by which nucleosynthesis takes to heavier species and would also indirectly constrain the $^{26}$Al content produced by supernovae thereby impacting the ratio of stellar $^{26}$Al/$^{60}$Fe, an important benchmark in supernovae nucleosynthesis. Despite significant progress on the subject there remains large uncertainties in one of the competing $^{26}$Al production channels which relies on the $^{25}$Al(p,$\gamma$)$^{26}$Si transition. This uncertainty is primarily characterized by the undetermined energy of the excited 3$^{+} \quad ^{26}$Si state which decays to the ground state of $^{25}$Al+p. To determine the resonance strength and energy of this transition an experiment is planned at the NSCL, which populates $^{26}$Si through the beta decay of $^{26}$P. Using an array of Ge clover detectors to measure the energies of the beta-delayed photons and their intensities, one could then determine $\Gamma_{\gamma}$, which then allows the calculation of the resonance strength (since $\Gamma_{p}$ is known), completing the decay scheme of the $^{25}$Al(p,$\gamma)^{26}$Si transition.