Determination of the astrophysical S factor for 11C(p,γ)12N from the 12N→11C+p asymptotic normalization coefficient

Details Determination of the astrophysical S factor for 11C(p,γ)12N from the 12N→11C+p asymptotic normalization coefficient Determination of the astrophysical S factor for 11C(p,γ)12N from the 12N→11C+p asymptotic normalization coefficient

Jan 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003phrvc..67a5804t&link_type=abstract

Physical Review C, vol. 67, Issue 1, id. 015804

Other

36

Nucleosynthesis In Novae, Supernovae, And Other Explosive Environments, Transfer Reactions, Radiative Capture, Elastic Scattering

Scientific paper

The evolution of very low-metallicity, massive stars depends critically on the amount of CNO nuclei that they produce. Alternative paths from the slow 3α process to produce CNO seed nuclei could change their fate. The 11C(p,γ)12N reaction is an important branch point in one such alternative path. At energies appropriate to stellar evolution of very low-metallicity, massive stars, nonresonant capture dominates the reaction rate. We have determined the astrophysical S factor for the 11C(p,γ)12N reaction using the asymptotic normalization coefficient for 12N→11C+p to fix the nonresonant capture rate. In our experiment, a 110 MeV 11C radioactive beam was used to study the14N(11C,12N)13C peripheral transfer reaction and the asymptotic normalization coefficient, (C12Npeff)2=(C12Np1/2)2+(C12Np3/2)2=1.73±0.25 fm-1, was extracted from the measured cross section. The contributions from the second resonance and interference effects were estimated using an R-matrix approach with the measured asymptotic normalization coefficient and the latest value for Γγ. We find the S factor for 11C(p,γ)12N is significantly larger than previous estimates. As a result, the required density for it to contribute is reduced, and more CNO material may be produced.

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