Proton capture on 34S in the astrophysical energy regime of O-Ne novae

Nuclear reaction sensitivity studies have shown that the final isotopic abundance of O-Ne nova nucleosynthesis is dependent on the 34S(p,γ)35Cl reaction at astrophysical energies corresponding to peak nova burning temperatures of 0.1–0.4 GK. Isotopic ratios of the S, Cl, and Ar products are all used...

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Bibliographic Details
Published in:Physical review. C 2021-05, Vol.103 (5)
Main Authors: Lovely, M., Lennarz, A., Connolly, D., Williams, M., Alcorta, M., Chen, A. A., Davids, B., Esker, N. E., Fry, C., Gillespie, S. A., Giri, R., Greife, U., Hussein, A., Hutcheon, D., Karpesky, J., Kroll, L., Liang, J., O'Malley, P. D., Paneru, S., Psaltis, A., Ruiz, C., Shotter, A. C.
Format: Article
Language:English
Subjects:
nuclear astrophysics
NUCLEAR PHYSICS AND RADIATION PHYSICS
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Summary:Nuclear reaction sensitivity studies have shown that the final isotopic abundance of O-Ne nova nucleosynthesis is dependent on the 34S(p,γ)35Cl reaction at astrophysical energies corresponding to peak nova burning temperatures of 0.1–0.4 GK. Isotopic ratios of the S, Cl, and Ar products are all used in various methods of cosmochemical analysis of presolar meteoritic grains. Due to the lack of direct experimental data, the 34S+p reaction rate has been estimated using statistical modeling or information from indirect nucleon transfer experiments. In order to provide direct reaction information, here the resonance strengths of several low energy resonances, Ec.m. = 272–495 keV, in the 34S(p,γ)35Cl reaction were measured for the first time in inverse kinematics using the DRAGON recoil separator located at TRIUMF, Canada’s Particle Accelerator Centre in Vancouver.
ISSN:2469-9985
2469-9993