Study of the direct ${}^{16}\mathrm{O}(p,\gamma {)}^{17}\mathrm{F}$ astrophysical capture reaction within a potential model approach

Abstract

A potential model is applied for the analysis of the astrophysical direct nuclear capture process ${}^{16}$O(p,$\gamma {)}^{17}$F. The phase-equivalent potentials of the Woods-Saxon form for the p${-}^{16}$O interaction are examined which reproduce the binding energies and the empirical values of ANC for the ${}^{17}$F(5/2${}^{+}$) ground and ${}^{17}$F(1/2${}^{+}$) ($E^{\ast }$=0.495 MeV) excited bound states from different sources. The best description of the experimental data for the astrophysical $S$ factor is obtained within the potential model which yields the ANC values of 1.043 fm${}^{-1/2}$ and 75.484 fm${}^{-1/2}$ for the ${}^{17}$F($5/2^{+}$) ground and ${}^{17}$F($1/2^{+}$) excited bound states, respectively. The zero-energy astrophysical factor $S(0)=9.321$ KeV b is obtained by using the asymptotic expansion method of D. Baye. The calculated reaction rates within the region up to 10${}^{10}$ K are in good agreement with those from the R-matrix approach and the Bayesian model in both absolute values and temperature dependence.

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References in corpus (6)

• New reaction rate for 16O(p,gamma)17F and its influence on the oxygen isotopic ratios in massive AGB stars
• Theoretical calculation of the $p-{}^6\mathrm{Li}$ radiative capture reaction
• Analysis of the ${}^3\mathrm{He}(\alpha ,\gamma {)}^7\mathrm{Be}$ and ${}^3\mathrm{H}(\alpha ,\gamma {)}^7\mathrm{Li}$ astrophysical direct capture reactions in a modified potential-model approach
• Astrophysical S factor and rate of ${}^7\mathrm{Be}(p,\gamma {)}^8\mathrm{B}$ direct capture reaction in a potential model
• Bayesian Estimation of the $S$ Factor and Thermonuclear Reaction Rate for ${}^{16}$O(p,$\gamma$)${}^{17}$F
• Study of nonlocality effects in direct capture reactions with Lagrange-mesh $R$-matrix method

Cited by in corpus (1)

• Variational neural-network solution of the two-body ${}^{17}\mathrm{F}$ proton-halo problem with a Coulomb--Whittaker tail