Determination of 11C(p,γ)12N astrophysical S-factor via measurement of 11C(d,n)12N reaction Original Research Article

Angular distribution of the 11C(d, n)12N reaction at Ecm=9.8 MeV was measured in inverse kinematics with the secondary 11C beam. The experimental data were analyzed with DWBA calculations and thereby the asymptotic normalization coefficient, View the MathML source, was extracted to be 2.86±0.91 fm−1 for the virtual decay View the MathML source. The zero energy astrophysical S-factor for the direct capture View the MathML source reaction was then derived to be 0.157±0.050 keV b. We have also estimated the contributions from resonant captures into the first- and second excited states of 12N and the interference between direct capture into the ground state and resonant capture into the second excited state. The temperature dependences of the direct capture, resonant capture and total reaction rates for View the MathML source were derived. The present work shows that the direct capture dominates the View the MathML source in the wide energy range of astrophysical interest except the ranges corresponding to two resonances.