Extrapolation of astrophysical S factors for the reaction 14N((p, γ) 15O to near-zero energies
Physics of Atomic Nuclei, 2012•Springer
The astrophysical S factors for the radiative-capture reaction 14 N (p, γ) 15 O in the region of
ultralow energies were calculated on the basis of the R-matrix approach. The values of the
radiative and protonic widths were fitted to new experimental data. The contribution of direct
radiative capture to bound states of the 15 O nucleus was determined with the aid of
asymptotic normalization coefficients, whose values were refined in the present study on the
basis of the results obtained from an analysis of the reaction 14 N (3 He, d) 15 O at three …
ultralow energies were calculated on the basis of the R-matrix approach. The values of the
radiative and protonic widths were fitted to new experimental data. The contribution of direct
radiative capture to bound states of the 15 O nucleus was determined with the aid of
asymptotic normalization coefficients, whose values were refined in the present study on the
basis of the results obtained from an analysis of the reaction 14 N (3 He, d) 15 O at three …
Abstract
The astrophysical S factors for the radiative-capture reaction 14N(p, γ)15O in the region of ultralow energies were calculated on the basis of the R-matrix approach. The values of the radiative and protonic widths were fitted to new experimental data. The contribution of direct radiative capture to bound states of the 15O nucleus was determined with the aid of asymptotic normalization coefficients, whose values were refined in the present study on the basis of the results obtained from an analysis of the reaction 14N(3He, d)15O at three different energies of incident helium ions. A value of S(0) = 1.79 ± 0.31 keV b was obtained for the total astrophysical S factor, and the reaction rate was determined for the process 14N(p, γ)15O.
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