Speaker
Description
Accurate modeling of classical nova nucleosynthesis is fundamentally dependent on the thermonuclear reaction rates of the nuclei involved. In particular it has been shown that the $^{30}$P(p,$\gamma$)$^{31}$S reaction rate is the largest source of uncertainty in the final abundance of nuclei created in a classical nova, involving an ONe white dwarf. The calculation of the $^{30}$P(p,$\gamma$)$^{31}$S reaction rate, at nova temperatures, requires knowledge of the spin and parity assignments and partial widths of the levels in $^{31}$S just above the proton threshold. To obtain the relevant nuclear data, a measurement of the $^{32}$S(p,d)$^{31}$S* reaction has been performed at the Texas A$\&$M Cyclotron Institue using a proton beam from the K150 cyclotron and a target consisting of ZnS deposited on a thin carbon backing. The newly commisioned, high-efficiency, particle-gamma array, Hyperion, was used in a configuration with 12 HPGe clover detectors and a dE-E telescope of segmented annular silicon detectors downstream of the target position for the detection of direct reaction products. In addition, a single silicon detector was placed upstream of the target for the detection of decay protons. Initial results from the experiment will be presented.
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This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of Nuclear Physic under contracts DE-FG02-96ER40983 (UTK), DE-AC05-00OR22725 (ORNL), DE-NA-0003780 (Notre Dame), DE-AC52-07NA27344 (LLNL), and DE-FG03-93ER40773 (TAMU), with additional support from The Welch Foundation, The National Science Foundation under PHY-1430152 (JINA-CEE), and the Laboratory Directed Research and Development Program of Oak Ridge National Laboratory.
