Asymptotic normalization coefficents and nuclear astrophysical processes

Details Asymptotic normalization coefficents and nuclear astrophysical processes Asymptotic normalization coefficents and nuclear astrophysical processes

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..dnp.cd008m&link_type=abstract

American Physical Society, Division of Nuclear Physics Fall Meeting, October 30 - November 1, 2003, Tucson, Arizona, MEETING ID:

Physics

Nuclear Physics

Scientific paper

The ANC method is a powerful indirect technique to obtain nuclear astrophysical information. This method is based on the determination of the ANCs from peripheral transfer reactions, both at above and sub-Coulomb energies, or from the elastic scattering. The ANC method is especially powerful when a subthreshold state contributes to the astrophysical radiative capture. In this case, the ANC method allows one to determine simultaneously the overall normalization of the direct capture astrophysical factor to the subthreshold state, the partial width of the subthreshold resonance and the channel part of the radiative width of the resonances decaying to the subthreshold state. We will illustrate the application of the ANC method for the analysis of the important astrophysical radiative capture reactions ^14N(p,γ)^15O and ^20Ne(p,γ)^21Na. The first one controls the energy production in the CNO cycle and the second one is the first reaction of the Ne-Na cycle. Both reactions are dominated by direct capture to a sub-threshold states. The ^3He(α, γ)^7Be emerges as one of the important hydrogen burning reactions whose reaction rate ought to be known with an accuracy of a few percent. We will discuss the sub-Coulomb transfer reaction ^3He(^6Li, d)^7Be as a tool to determine the astrophysical factor for ^3He(α,γ)^7Be.

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