Astrophysical factor for the CNO cycle radiative capture reaction^15N(p,γ)^16O

Details Astrophysical factor for the CNO cycle radiative capture reaction^15N(p,γ)^16O Astrophysical factor for the CNO cycle radiative capture reaction^15N(p,γ)^16O

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aps..dnp.da064p&link_type=abstract

American Physical Society, 2007 Annual Meeting of the Division of Nuclear Physics, October 10-13,2007, abstract #DA.064

Physics

Nuclear Physics

Scientific paper

The reaction ^15N(p,γ) ^16O leaks from CN cycle and determines the oxygen isotopes generated in CNO tri-cycle. Direct measurements of the astrophysical S(E) factor for this reaction were reported [1]. The analysis [1] assumes that the reaction is dominated by resonances at Ecm=312,and,64,keV, and direct capture to the ground state of ^16O. The ANCs for bound states of ^16O have been measured in reaction ^15N( ^3He,d) ^16O [2]. Using these ANCs, the astrophysical factor for ^15N(p,γ) ^16O has been calculated by the R-matrix approach. The proton and α widths of two resonances were determined from the fit to the direct data for ^15N(p,α) ^12C [3] and used to calculate the S(E) factor for ^15N(p,γ) ^16O. Radiative were varied within experimental uncertainty to fit to the direct data for ^15N(p,γ) ^16O. The calculated S(E) factor is S(0)=38,keVb if we fit the S(E) factor at the resonance peaks; this is significantly smaller than the value S(0)=64±6 keVb reported in [1]. Hence, one reaction ^15N(p,γ) ^16O occurs for almost 1500 CN cycles, rather than 880 cycles as estimated in [1]. The problem with fitting the data from [1] at resonance peaks and small energies necessitates re-measurement at lower energies of this reaction. [1] Rolfs, C., and Rodney, W.S., Nucl. Phys. A235 (1974) 450. [2] A. M. Mukhamedzhanov, P. Bem, V. Burjan et al., Phys. Rev. C (will be submitted). [3] A. Redder et al., Z. Phys. A305, 325 (1982).

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