Proton Emission from $^{31}$S and the Astrophysical $^{30}$P$(p,\gamma)^{31}$S Reaction
ORAL
Abstract
The $^{30}$P$(p,\gamma)^{31}$S reaction rate has been identified as the largest remaining source of uncertainty in the abundances of intermediate-mass nuclei produced in classical nova explosions involving oxygen-neon white dwarfs, and is critical to interpreting the origin of certain meteoritic presolar grains. To inform the astrophysical proton capture rate, the $^{32}$S$(p,d)^{31}$S reaction has been used to populate proton unbound states in $^{31}$S. The Hyperion array was used to measure the reaction deuterons in coincidence with decay protons and γ rays. Angular correlations between the reaction products and decay protons have been measured and used to constrain the angular momentum of states in $^{31}$S above the proton threshold. In addition, proton-decay branching ratios have been measured for these states and used to inform resonance strengths.
*U.S. DOE under DE-FG02-96ER40983 (UTK), DEAC05-00OR22725 (ORNL), DE-NA-0003780 (Notre Dame), DE-AC52-07NA27344 (LLNL), and DE-FG03-93ER40773 (TAMU), The Welch Foundation, The NSF under PHY-1430152 (JINA-CEE). Laboratory Directed Research and Development Program of ORNL
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