Improved Direct Measurement of the 64.5 keV Resonance Strength in theO17(p,α)N14Reaction at LUNA

• DOI: 10.1103/physrevlett.117.142502
• Publication Date: 2016-09-27T22:08:34Z
• Authors: C. G. Bruno; D. A. Scott; M. Aliotta; A. Formicola; A. Best; A. Boeltzig; D. Bemmerer; C. Broggini; A. Caciolli; F. Cavanna; G. F. Ciani; P. Corvisiero; T. Davinson; R. Depalo; A. Di Leva; Z. Elekes; F. Ferraro; Zs. Fülöp; G. Gervino; A. Guglielmetti; C. Gustavino; Gy. Gyürky; G. Imbriani; M. Junker; R. Menegazzo; V. Mossa; F. R. Pantaleo; D. Piatti; P. Prati; E. Somorjai; O. Straniero; F. Strieder; T. Szücs; M. P. Takács; D. Trezzi
• Keywords: Asymptotic giant branch

The ^{17}O(p,α)^{14}N reaction plays a key role in various astrophysical scenarios, from asymptotic giant branch stars to classical novae. It affects the synthesis of rare isotopes such as ^{17}O and ^{18}F, which can provide constraints on models. A new direct determination E_{R}=64.5 keV resonance strength performed at Laboratory for Underground Nuclear Astrophysics (LUNA) accelerator has led most accurate value date ωγ=10.0±1.4_{stat}±0.7_{syst} neV, thanks significant background reduction underground generally improved experimental conditions. (bare) proton partial width corresponding state E_{x}=5672 ^{18}F is Γ_{p}=35±5_{stat}±3_{syst} neV. This about factor 2 higher than previously estimated, thus leading increase ^{17}O(p, α)^{14}N rate temperatures relevant shell hydrogen burning red stars. implies lower ^{17}O/^{16}O ratios, with important implications interpretation observables these