Improving the {sup 33}S(p,{gamma}){sup 34}Cl Reaction Rate for Models of Classical Nova Explosions

Journal Article · Fri Oct 28 00:00:00 EDT 2011 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.3628377· OSTI ID:21612046

Parikh, A; Faestermann, Th; Kruecken, R; Bildstein, V; Bishop, S; Eppinger, K; Herlitzius, C; Lepyoshkina, O; Maierbeck, P; Seiler, D; Wimmer, K ^[1]; Hertenberger, R; Wirth, H -F ^[2]; Fallis, J; Hager, U; Hutcheon, D; Ruiz, Ch; Buchmann, L; Ottewell, D ^[3]; Freeman, B ^[4]

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1. Physik Department E12, Technische Universitaet Muenchen, D-85748, Garching (Germany)
2. Fakultaet fuer Physik, Ludwig-Maximilians-Universitaet Muenchen, D-85748 Garching (Germany)
3. TRIUMF, Vancouver, BC, V6T 2A3 (Canada)
4. Center for Experimental Nuclear Physics and Astrophysics, University of Washington, Seattle, WA 98195 (United States)

Reduced uncertainty in the thermonuclear rate of the {sup 33}S(p,{gamma}){sup 34}Cl reaction would help to improve our understanding of nucleosynthesis in classical nova explosions. At present, models are generally in concordance with observations that nuclei up to roughly the calcium region may be produced in these explosive phenomena; better knowledge of this rate would help with the quantitative interpretation of nova observations over the S-Ca mass region, and contribute towards the firm establishment of a nucleosynthetic endpoint. As well, models find that the ejecta of nova explosions on massive oxygen-neon white dwarfs may contain as much as 150 times the solar abundance of {sup 33}S. This characteristic isotopic signature of a nova explosion could possibly be observed through the analysis of microscopic grains formed in the environment surrounding a nova and later embedded within primitive meteorites. An improved {sup 33}S(p,{gamma}){sup 34}Cl rate (the principal destruction mechanism for {sup 33}S in novae) would help to ensure a robust model prediction for the amount of {sup 33}S that may be produced. Finally, constraining this rate could confirm or rule out the decay of an isomeric state of {sup 34}Cl(E{sub x} = 146 keV, t{sub 1/2} = 32 m) as a source for observable gamma-rays from novae. We have performed several complementary experiments dedicated to improving our knowledge of the {sup 33}S(p,{gamma}){sup 34}Cl rate, using both indirect methods (measurement of the {sup 34}S({sup 3}He,t){sup 34}Cl and {sup 33}S({sup 3}He,d){sup 34}Cl reactions with the Munich Q3D spectrograph) and direct methods (in normal kinematics at CENPA, University of Washington, and in inverse kinematics with the DRAGON recoil mass separator at TRIUMF). Our results will be used with nova models to facilitate comparisons of model predictions with present and future nova observables.

• OSTI ID: 21612046
• Journal Information: AIP Conference Proceedings, Vol. 1377, Issue 1; Conference: FINUSTAR 3 Conference on frontiers in nuclear structure, astrophysics, and reactions, Rhodes (Greece), 23-27 Aug 2010; Other Information: DOI: 10.1063/1.3628377; (c) 2011 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
CHLORINE 34
COMPARATIVE EVALUATIONS
COSMIC PHOTONS
DEUTERONS
ELEMENT ABUNDANCE
GAMMA RADIATION
HELIUM 3
HELIUM 3 REACTIONS
KEV RANGE
NOVA MODEL
NOVAE
NUCLEOSYNTHESIS
PARTICLE KINEMATICS
PROTON REACTIONS
RECOILS
SULFUR 33 TARGET
TRITONS
WHITE DWARF STARS
ABUNDANCE
BARYON REACTIONS
BETA DECAY RADIOISOTOPES
BETA-PLUS DECAY RADIOISOTOPES
BINARY STARS
BOSONS
CHARGED PARTICLES
CHARGED-PARTICLE REACTIONS
CHLORINE ISOTOPES
COSMIC RADIATION
DWARF STARS
ELECTROMAGNETIC RADIATION
ELEMENTARY PARTICLES
ENERGY RANGE
ERUPTIVE VARIABLE STARS
EVALUATION
EVEN-ODD NUCLEI
HADRON REACTIONS
HELIUM ISOTOPES
IONIZING RADIATIONS
ISOMERIC TRANSITION ISOTOPES
ISOTOPES
LIGHT NUCLEI
MASSLESS PARTICLES
MATHEMATICAL MODELS
MINUTES LIVING RADIOISOTOPES
NUCLEAR REACTIONS
NUCLEI
NUCLEON REACTIONS
ODD-ODD NUCLEI
PARTICLE MODELS
PHOTONS
RADIATIONS
RADIOISOTOPES
SECONDS LIVING RADIOISOTOPES
STABLE ISOTOPES
STARS
SYNTHESIS
TARGETS
VARIABLE STARS