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

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 17F(p, γ)18Ne. The dominant contribution to the cross-section at very low-energies is due to M1 transitions whose magnitude is controlled by a weakly bound state at the excitation energy .