Constraining the astrophysical $^{23}$Mg(p,$\gamma$)$^{24}$Al reaction rate using the $^{23}$Na(d,p)$^{24}$Na reaction

The $^{23}$Mg(p,$\gamma$)$^{24}$Al reaction provides an escape from the Ne-Na cycle in classical novae and is therefore important in understanding nova nucleosynthesis in the $A>20$ mass range. Although several resonances may contribute to the overall rate at novae temperatures, the resonance at $\sim$475 keV is thought to be dominant. The strength of this resonance has been directly measured using a radioactive $^{23}$Mg beam impinging on a windowless H$_2$ gas target; however, recent high-precision $^{24}$Al mass measurements have called this result into question. Here we make an indirect measurement using the $^{23}$Na(d,p)$^{24}$Na reaction in inverse kinematics to study the mirror state of the $\sim$475 keV resonance in $^{24}$Na. The experiment, performed at the Texas A\&M Cyclotron Institute, utilized the TIARA silicon array, four HPGe detectors, and the MDM spectrometer to measure the excited states of the $^{24}$Na nucleus. Preliminary results from the experiment will be presented along with progress from the ongoing analysis.