Astrophysical S factors for CNO reactions ^11C(p,γ)^12N and ^14N(p,γ)^15O from asymptotic normalization coefficients

Details Astrophysical S factors for CNO reactions ^11C(p,γ)^12N and ^14N(p,γ)^15O from asymptotic normalization coefficients Astrophysical S factors for CNO reactions ^11C(p,γ)^12N and ^14N(p,γ)^15O from asymptotic normalization coefficients

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..dnp.de002m&link_type=abstract

American Physical Society, 2002 Fall Meeting of the Division of Nuclear , abstract #DE.002

Astronomy and Astrophysics

Astrophysics

Scientific paper

The ^11C(p,γ)^12N reaction, which can affect the evolution of the supermassive stars, is dominated by the direct capture and its interference with the second resonance. The normalization of the direct capture term is governed by the asymptotic normalization coefficient (ANC) for ^12N ^11C + p. This ANC has been determined from the ^14N(^11C(110 MeV), ^12N)^13C reaction. Using the determined ANC we find the astrophysical S factor for ^11C(p,γ)^12N to be significantly larger than the previous estimates. The ^14N(p,γ)^15O capture controls its energy generation. The reaction is dominated by the direct captures to different states of ^15O and resonances. The main uncertainty is caused by the fourth excited state 3/2^+ in ^15O. This state can contribute as a subthreshold bound state and subthreshold resonance. We present here the results of the measurements of the ANC's for ^14N +p ^15O leading to the ground and 5 excited sates in ^15O using the reaction ^14N(^3He(26.3 MeV),d)^15O. We calculated the astrophysical S factor for ^14N(p,γ)^15O and reaction rates. Our analysis favors a low value of the astrophysical factor.

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