New measurements of low-energy resonances in the ${}^{22}\mathbf{Ne}(p,\gamma ){}^{23}\mathbf{Na}$ reaction

Journal Article · Wed Jan 18 23:00:00 EST 2017 · Physical Review C

DOI: https://doi.org/10.1103/PhysRevC.95.015806 · OSTI ID:1600490

Kelly, K. J. ^[1]; Champagne, A. E. ^[2]; Downen, L. N. ^[2]; Dermigny, J. R. ^[2]; Hunt, S. ^[2]; Iliadis, C. ^[2]; Cooper, A. L. ^[2]

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1. Univ. of North Carolina, Chapel Hill, NC (United States); Triangle Univ. Nuclear Lab., Durham, NC (United States); Duke Univ., Durham, NC (United States); Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Univ. of North Carolina, Triangle Universities Nuclear Laboratory
2. Univ. of North Carolina, Chapel Hill, NC (United States); Triangle Univ. Nuclear Lab., Durham, NC (United States); Duke Univ., Durham, NC (United States)

The ${}_{22}\mathrm{Ne}(p,\gamma ){}_{23}\mathrm{Na}$ reaction is one of the most uncertain reactions in the NeNa cycle and plays a crucial role in the creation of ${}_{23}\mathrm{Na}$, the only stable Na isotope. Uncertainties in the low-energy rates of this and other reactions in the NeNa cycle lead to ambiguities in the nucleosynthesis predicted from models of thermally pulsing asymptotic giant branch (AGB) stars. This in turn complicates the interpretation of anomalous Na-O trends in globular cluster evolutionary scenarios. Prior studies of the ${}_{22}\mathrm{Ne}(p,\gamma ){}_{23}\mathrm{Na}$, ${}_{22}\mathrm{Ne}({}_3\mathrm{He},d){}_{23}\mathrm{Na}$, and ${}_{12}\mathrm{C}({}_{12}\mathrm{C},p){}_{23}\mathrm{Na}$ reactions disagree on the strengths, spins, and parities of low-energy resonances in ${}_{23}\mathrm{Na}$ and the direct-capture ${}_{22}\mathrm{Ne}(p,\gamma ){}_{23}\mathrm{Na}$ reaction rate contains large uncertainties as well. Here, we present new measurements of resonances at $E_r^{\text{c.m.}}=417$, 178, and 151 keV and of the direct-capture process in the ${}_{22}\mathrm{Ne}(p,\gamma ){}_{23}\mathrm{Na}$ reaction. The resulting total ${}_{22}\mathrm{Ne}(p,\gamma ){}_{23}\mathrm{Na}$ rate is approximately a factor of 20 higher than the rate listed in a recent compilation at temperatures relevant to hot-bottom burning in AGB stars. Although our rate is close to that derived from a recent ${}_{22}\mathrm{Ne}(p,\gamma ){}_{23}\mathrm{Na}$ measurement by Cavanna et al. in 2015, we find that this large rate increase results in only a modest 18% increase in the ${}_{23}\mathrm{Na}$ abundance predicted from a 5 ${\mathrm{M}}_{\odot }$ thermally pulsing AGB star model from Ventura and D'Antona (2005). The estimated astrophysical impact of this rate increase is in marked contrast to the factor of $~3$ increase in ${}_{23}\mathrm{Na}$ abundance predicted by Cavanna et al. and is attributed to the interplay between the ${}_{23}\mathrm{Na}(p,\alpha ){}_{20}\mathrm{Ne}$ and ${}_{20}\mathrm{Ne}(p,\gamma ){}_{21}\mathrm{Na}$ reactions, both of which remain fairly uncertain at the relevant temperature range.

• Research Organization: Univ. of North Carolina, Chapel Hill, NC (United States)
• Sponsoring Organization: USDOE Office of Science (SC), Nuclear Physics (NP) (SC-26)
• Grant/Contract Number: FG02-97ER41041
• OSTI ID: 1600490
• Journal Information: Physical Review C, Journal Name: Physical Review C Journal Issue: 1 Vol. 95; ISSN PRVCAN; ISSN 2469-9985
• Publisher: American Physical Society (APS)Copyright Statement
• Country of Publication: United States
• Language: English