Branches of {sup 33}S(p,{gamma}){sup 34}Cl at oxygen-neon nova temperatures
- Department of Physics, University of Washington, Seattle, Washington 98195-1560 (United States)
- Physik Department E12, Technische Universitaet Muenchen, D-85748 Garching (Germany)
Recent simulations of classical novae on oxygen-neon white-dwarf stars indicate that the isotopic ratio {sup 32}S/{sup 33}S has the potential to be a remarkable indicator of presolar grains of nova origin. The {sup 33}S(p,{gamma}){sup 34}Cl reaction influences this ratio directly by destroying {sup 33}S in novae. Additionally, {beta}-delayed {gamma} rays from the metastable state of {sup 34}Cl (t{sub 1/2}=32 min) have been suggested to be potential nova observables. We have measured the branches for known {sup 33}S(p,{gamma}){sup 34}Cl 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.
- OSTI ID:
- 21499645
- Journal Information:
- Physical Review. C, Nuclear Physics, Vol. 83, Issue 4; Other Information: DOI: 10.1103/PhysRevC.83.048801; (c) 2011 American Institute of Physics; ISSN 0556-2813
- Country of Publication:
- United States
- Language:
- English
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BRANCHING RATIO
CHLORINE 34
DATA COVARIANCES
GAMMA DECAY
GAMMA RADIATION
ISOTOPE RATIO
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NEON
NOVAE
OXYGEN
PROTON REACTIONS
RESONANCE
SIMULATION
SULFUR 33 TARGET
WHITE DWARF STARS
BARYON REACTIONS
BETA DECAY RADIOISOTOPES
BETA-PLUS DECAY RADIOISOTOPES
BINARY STARS
CHARGED-PARTICLE REACTIONS
CHLORINE ISOTOPES
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ELECTROMAGNETIC RADIATION
ELEMENTS
ENERGY LEVELS
ERUPTIVE VARIABLE STARS
EXCITED STATES
FLUIDS
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IONIZING RADIATIONS
ISOMERIC TRANSITION ISOTOPES
ISOTOPES
LIGHT NUCLEI
MINUTES LIVING RADIOISOTOPES
NONMETALS
NUCLEAR DECAY
NUCLEAR REACTIONS
NUCLEI
NUCLEON REACTIONS
ODD-ODD NUCLEI
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