Description of the 17F(p, γ)18Ne radiative capture reaction in the continuum shell model

Abstract The shell model embedded in the continuum is applied to calculate the astrophysical S-factor and the reaction rate for the radiative proton capture reaction 17 F(p, γ ) 18 Ne. The dominant contribution to the cross-section at very low-energies is due to M1 transitions J i π = 2 + → J f π = 2 1 + whose magnitude is controlled by a weakly bound 2 2 + state at the excitation energy E x = 3.62 MeV .