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Bennett MB, Wrede C, Brown BA, et al. Isospin Mixing Reveals ^{30}P(p,γ)^{31}S Resonance Influencing Nova Nucleosynthesis. Phys Rev Lett. 2016;116(10):102502doi: 10.1103/PhysRevLett.116.102502.
Bennett, M. B., Wrede, C., Brown, B. A., Liddick, S. N., Pérez-Loureiro, D., Bardayan, D. W., Chen, A. A., Chipps, K. A., Fry, C., Glassman, B. E., Langer, C., Larson, N. R., McNeice, E. I., Meisel, Z., Ong, W., O'Malley, P. D., Pain, S. D., Prokop, C. J., Schatz, H., Schwartz, S. B., Suchyta, S., Thompson, P., Walters, M., & Xu, X. (2016). Isospin Mixing Reveals ^{30}P(p,γ)^{31}S Resonance Influencing Nova Nucleosynthesis. Physical review letters, 116(10), 102502. https://doi.org/10.1103/PhysRevLett.116.102502
Bennett, M B, et al. "Isospin Mixing Reveals ^{30}P(p,γ)^{31}S Resonance Influencing Nova Nucleosynthesis." Physical review letters vol. 116,10 (2016): 102502. doi: https://doi.org/10.1103/PhysRevLett.116.102502
Bennett MB, Wrede C, Brown BA, Liddick SN, Pérez-Loureiro D, Bardayan DW, Chen AA, Chipps KA, Fry C, Glassman BE, Langer C, Larson NR, McNeice EI, Meisel Z, Ong W, O'Malley PD, Pain SD, Prokop CJ, Schatz H, Schwartz SB, Suchyta S, Thompson P, Walters M, Xu X. Isospin Mixing Reveals ^{30}P(p,γ)^{31}S Resonance Influencing Nova Nucleosynthesis. Phys Rev Lett. 2016 Mar 11;116(10):102502. doi: 10.1103/PhysRevLett.116.102502. Epub 2016 Mar 08. PMID: 27015475.
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Phys Rev Lett. 2016 Mar 11;116(10):102502. doi: 10.1103/PhysRevLett.116.102502. Epub 2016 Mar 08.

Isospin Mixing Reveals ^{30}P(p,γ)^{31}S Resonance Influencing Nova Nucleosynthesis.

Physical review letters

M B Bennett, C Wrede, B A Brown, S N Liddick, D Pérez-Loureiro, D W Bardayan, A A Chen, K A Chipps, C Fry, B E Glassman, C Langer, N R Larson, E I McNeice, Z Meisel, W Ong, P D O'Malley, S D Pain, C J Prokop, H Schatz, S B Schwartz, S Suchyta, P Thompson, M Walters, X Xu

Affiliations

  1. Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
  2. National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  3. Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA.
  4. Department of Chemistry, Michigan State University, East Lansing, Michigan 48824, USA.
  5. Department of Physics, University of Notre Dame, Notre Dame, Indiana 46556, USA.
  6. Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada.
  7. Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USA.
  8. Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA.
  9. Department of Geology and Physics, University of Southern Indiana, Evansville, Indiana 47712, USA.

PMID: 27015475 DOI: 10.1103/PhysRevLett.116.102502

Abstract

The thermonuclear ^{30}P(p,γ)^{31}S reaction rate is critical for modeling the final elemental and isotopic abundances of ONe nova nucleosynthesis, which affect the calibration of proposed nova thermometers and the identification of presolar nova grains, respectively. Unfortunately, the rate of this reaction is essentially unconstrained experimentally, because the strengths of key ^{31}S proton capture resonance states are not known, largely due to uncertainties in their spins and parities. Using the β decay of ^{31}Cl, we have observed the β-delayed γ decay of a ^{31}S state at E_{x}=6390.2(7)  keV, with a ^{30}P(p,γ)^{31}S resonance energy of E_{r}=259.3(8)  keV, in the middle of the ^{30}P(p,γ)^{31}S Gamow window for peak nova temperatures. This state exhibits isospin mixing with the nearby isobaric analog state at E_{x}=6279.0(6)  keV, giving it an unambiguous spin and parity of 3/2^{+} and making it an important l=0 resonance for proton capture on ^{30}P.

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