Recent simulations of classical novae on oxygen-neon white-dwarf stars indicate that the isotopic ratio 32S/33S has the potential to be a remarkable indicator of presolar grains of nova origin. The 33S(p,\gamma)34Cl reaction influences this ratio directly by destroying 33S in novae. Additionally, \beta-delayed \gamma-rays from the metastable state of 34Cl (t_{1/2} = 32 min) have been suggested to be potential nova observables. We have measured the branches for known 33S(p,\gamma)34Cl resonances that are activated at temperatures relevant to oxygen-neon novae. We provide the first reliable uncertainties on these branches and the first upper limits for several previously unmeasured branches.
@article{arxiv.1101.0643,
title = {Branches of 33S(p,{\gamma})34Cl at Oxygen-Neon Nova Temperatures},
author = {B. M. Freeman and C. Wrede and B. G. Delbridge and A. Garcia and A. Knecht and A. Parikh and A. L. Sallaska},
journal= {arXiv preprint arXiv:1101.0643},
year = {2011}
}