Constraining the S factor of 15N(p,g)16O at Astrophysical Energies

Abstract

The 15N(p,g)16O reaction represents a break out reaction linking the first and second cycle of the CNO cycles redistributing the carbon and nitrogen abundances into the oxygen range. The reaction is dominated by two broad resonances at Ep = 338 keV and 1028 keV and a Direct Capture contribution to the ground state of 16O. Interference effects between these contributions in both the low energy region (Ep < 338 keV) and in between the two resonances (338 <Ep < 1028 keV) can dramatically effect the extrapolation to energies of astrophysical interest. To facilitate a reliable extrapolation the 15N(p,g)16O reaction has been remeasured covering the energy range from Ep=1800 keV down to 130 keV. The results have been analyzed in the framework of a multi-level R-matrix theory and a S(0) value of 39.6 keV b has been found.

arXiv comment15 pages, 9 figures

References in corpus (6)

• S-factor of 14N(p,gamma)15O at astrophysical energies
• The bottleneck of the CNO burning and the age of the Globular Clusters
• LUNA: a Laboratory for Underground Nuclear Astrophysics
• Direct measurement of the 14N(p,g)15O S-factor
• Feasibility of low energy radiative capture experiments at the LUNA underground accelerator facility
• Direct measurement of the 15N(p,gamma)16O total cross section at novae energies

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• A new approach to monitor 13C-targets degradation in situ for 13C(alpha,n)16O cross-section measurements at LUNA
• Exploring Stars in Underground Laboratories: Challenges and Solutions
• Solar fusion III: New data and theory for hydrogen-burning stars
• Shell and explosive hydrogen burning
• Study of the neutron and proton capture reactions 10,11b(n, g), 11b(p, g), 14c(p, g), and 15n(p, g) at thermal and astrophysical energies
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• Radiative proton capture on ${}^{15}\mathrm{N}$ within effective field theory