Branches of 33S(p,γ)34Cl at Oxygen-Neon Nova Temperatures

Details Branches of 33S(p,γ)34Cl at Oxygen-Neon Nova Temperatures Branches of 33S(p,γ)34Cl at Oxygen-Neon Nova Temperatures

2011-01-04

arxiv.org/abs/1101.0643v2

Phys.Rev.C83:048801,2011

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

Scientific paper

10.1103/PhysRevC.83.048801

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.

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