Studying the $^{30}$P(p,$\gamma$)$^{31}$S reaction using the $^{31}$P($^{3}$He,t)$^{31}$S$^{*}$(p)$^{30}$P reaction

Enriched isotopic abundance ratios of $^{30}$Si/$^{28}$Si in several presolar SiC and graphite grains qualitatively indicate oxygen-neon (ONe) nova origins but fall short of ONe nova model predictions by factors of 20-90. The $^{30}$P(p,$\gamma$)$^{31} $S reaction rate uncertainty in ONe novae spans four orders of magnitude through which the predicted amount of ejected $^{30} $Si can vary by a factor of 100. By measuring the $^{31}$P($^{3}$He,t)$^{31}$S$^{*}$(p)$^{30}$P reaction we have determined the energies of astrophysically relevant $^{31}$S excited states to $\pm$ 3 keV, and have found one new resonance. Proton branching ratios have been constrained by detecting decay protons in coincidence with tritons. Implications for the $^{30}$P(p,$\gamma$)$^{31}$S reaction rate, $^{30}$Si production, and S-Ca production in ONe novae will be presented.