Abstract
Isotopic abundance ratios of 30Si/28Si found in presolar SiC grains of suspected nova origin agree qualitatively with proposed oxygen-neon (ONe) nova composition but fail to agree quantitatively with ejecta predictions made by hydrodynamic ONe nova models. The Astrophysical 30P(p,γ)31S reaction rate is a key quantity used in nova models that predict isotopic abundances produced during nucleosynthesis leading up to the outburst. Currently, there is a large uncertainty in the rate at nova temperatures (0.1 < T < 0.4 GK) causing the predicted 30Si abundance ratio to vary by a factor of 4. The 30P(p,γ)31S reaction rate can be determined indirectly by measuring triton momenta from 32S(d,t)31S reactions. 31S Resonant states measured up to 600 keV above the proton threshold of 6131 keV and within the Gamow window which contribute most significantly to the rate can then be used to re-evaluate the rate for nova temperatures and reduce the uncertainty.
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