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

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

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003nupha.728..275l&link_type=abstract

Nuclear Physics A, Volume 728, Issue 1-2, p. 275-284.

Physics

Nuclear Physics

9

2H(11C, 12N), Ecm=9.8 Mev, Σ(Θ), Asymptotic Normalization Coefficient, 11C(P, Γ), E=Low, Astrophysical S-Factor, Reaction Mechanism Features, Dwba Analysis.

Scientific paper

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, (Cpeff12N)2=(Cp1/212N)2+(Cp3/212N)2, was extracted to be 2.86+/-0.91 fm-1 for the virtual decay 12N-->11C+p. The zero energy astrophysical S-factor for the direct capture 11C(p,γ)12N reaction was then derived to be 0.157+/-0.050 keVb. 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 11C(p,γ)12N were derived. The present work shows that the direct capture dominates the 11C(p,γ)12N in the wide energy range of astrophysical interest except the ranges corresponding to two resonances.

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