Astrophysical S-factor of the ${}^{14}\text{N(p,}\gamma {\text{)}}^{15}\text{O}$ reaction at 0.4 -- 1.3\,MeV

Abstract

The ${}^{14}\text{N(p,}\gamma {\text{)}}^{15}\text{O}$ reaction is the slowest reaction of the carbon-nitrogen cycle of hydrogen burning and thus determines its rate. The precise knowledge of its rate is required to correctly model hydrogen burning in asymptotic giant branch stars. In addition, it is a necessary ingredient for a possible solution of the solar abundance problem by using the solar ${}^{13}$N and ${}^{15}$O neutrino fluxes as probes of the carbon and nitrogen abundances in the solar core. After the downward revision of its cross section due to a much lower contribution by one particular transition, capture to the ground state in ${}^{15}$O, the evaluated total uncertainty is still 8\%, in part due to an unsatisfactory knowledge of the excitation function over a wide energy range. The present work reports precise S-factor data at twelve energies between 0.357-1.292~MeV for the strongest transition, capture to the 6.79~MeV excited state in ${}^{15}$O, and at ten energies between 0.479-1.202~MeV for the second strongest transition, capture to the ground state in ${}^{15}$O. An R-matrix fit is performed to estimate the impact of the new data on astrophysical energies. The recently suggested slight enhancement of the 6.79~MeV transition at low energy could not be confirmed. The present extrapolated zero-energy S-factors are $S_{6.79}(0)$~=~1.24$\pm$0.11~keV~barn and $S_{\mathrm{GS}}(0)$~=~0.19$\pm$0.05~keV~barn.

arXiv commentSubmitted to Phys. Rev. C

References in corpus (26)

• The chemical composition of the Sun
• Solar Chemical Abundances Determined with a CO5BOLD 3D Model Atmosphere
• Solar fusion cross sections II: the pp chain and CNO cycles
• Solar Fusion Cross Sections
• The R-matrix theory
• New Solar Composition: The Problem With Solar Models Revisited
• Current Status and Future Prospects of the SNO+ Experiment
• S-factor of 14N(p,gamma)15O at astrophysical energies
• Solar models with accretion. I. Application to the solar abundance problem
• The bottleneck of the CNO burning and the age of the Globular Clusters
• First measurement of the 14N(p,gamma)15O cross section down to 70 keV
• CN-Cycle Solar Neutrinos and Sun's Primordial Core Metalicity
• Letter of Intent: Jinping Neutrino Experiment
• Direct measurement of the 14N(p,g)15O S-factor
• Precision study of ground state capture in the 14N(p,gamma)15O reaction
• Nuclear Reaction Rates and Carbon Star Formation
• Nuclear Reaction Rate Uncertainties and Astrophysical Modeling. II. Carbon Yields from Low-mass Giants
• The 14N(p,gamma)15O reaction studied with a composite germanium detector
• Resonance strengths in the 14N(p, γ)15O and 15N(p, αγ)12C reactions
• Strengths of the resonances at 436, 479, 639, 661, and 1279 keV in the ${}^{22}$Ne(p,$\gamma$)${}^{23}$Na reaction
• The ${}^{14}N(p,\gamma {)}^{15}O$ reaction, solar neutrinos and the age of the globular clusters
• Constraining Big Bang lithium production with recent solar neutrino data
• The resonance triplet at E_alpha = 4.5 MeV in the 40Ca(alpha,gamma)44Ti reaction
• Strength of the $E_{\text{p}}$=1.842 MeV resonance in the ${}^{40}$Ca(p,$\gamma$)${}^{41}$Sc reaction revisited
• Absolute hydrogen depth profiling using the resonant ${}^1$H(${}^{15}$N,$\alpha \gamma$)${}^{12}$C nuclear reaction
• Progress of the Felsenkeller shallow-underground accelerator for nuclear astrophysics

Cited by in corpus (13)

• The Future of Solar Neutrinos
• Background in $\gamma$-ray detectors and carbon beam tests in the Felsenkeller shallow-underground accelerator laboratory
• Solar fusion III: New data and theory for hydrogen-burning stars
• Resonance strengths in the 14N(p,gamma)15O astrophysical key reaction measured with activation
• The K2 M67 Study: Precise Mass for a Turnoff Star in the Old Open Cluster M67
• Measurement of the ${}^2$H($p,\gamma$)${}^3$He S-factor at 265-1094keV
• Activation cross section measurement of the 14N(p,gamma)15O astrophysical key reaction
• Lifetime measurements of excited states in ${}^{15}$O
• The Felsenkeller shallow-underground laboratory for nuclear astrophysics
• Reaction Rate Of p14N --> 15Ogamma Capture To All Bound States In Potential Cluster Model
• Radiative Capture of proton 14N(p,γ) 15O at Low Energy
• Study of the ${}^{20}$Ne($p,\gamma$)${}^{21}$Na reaction at LUNA
• Investigating the impact of Solar Fusion III reaction rates on helioseismic constraints and solar neutrino fluxes