S-factor of 14N(p,γ)15O at astrophysical energies⋆

  title={S-factor of 14N(p,$\gamma$)15O at astrophysical energies⋆},
  author={Gianluca Imbriani and Heide Costantini and Alba Formicola and Alberto Vomiero and Carmen Angulo and Daniel Bemmerer and Roberto Bonetti and Carlo Broggini and Federica Confortola and Pietro Corvisiero and J. Cruz and Pierre Descouvemont and Zs. F{\"u}l{\"o}p and Gianpiero Gervino and Alessandra Guglielmetti and C Gustavino and Gy. Gy{\"u}rky and A. P. Jesus and Markus Junker and J. N. Klug and Alberto Lemut and R. Menegazzo and Paolo Prati and Vincent Roca and Claus E. Rolfs and Mario R. Romano and C. Rossi-Alvarez and F. Schuemann and D. Sch{\"u}rmann and E. Somorjai and Oscar Straniero and Frank Strieder and Filippo Terrasi and H. P. Trautvetter},
  journal={The European Physical Journal A - Hadrons and Nuclei},
Abstract.The astrophysical S(E) factor of 14N(p,γ)15O has been measured for effective center-of-mass energies between Eeff = 119 and 367 keV at the LUNA facility using TiN solid targets and Ge detectors. The data are in good agreement with previous and recent work at overlapping energies. R-matrix analysis reveals that due to the complex level structure of 15O the extrapolated S(0) value is model dependent and calls for additional experimental efforts to reduce the present uncertainty in S(0… Expand
Extrapolation of astrophysical S factors for the reaction 14N((p, γ) 15O to near-zero energies
The astrophysical S factors for the radiative-capture reaction 14N(p, γ)15O in the region of ultralow energies were calculated on the basis of the R-matrix approach. The values of the radiative andExpand
Proton capture by 14N at astrophysical energies
Calculations are reported for low energy, proton capture by 14N with the recoil corrected continuum shell model. An interaction from a fit to Cohen and Kurath (6–16) p-shell matrix elements and ReidExpand
Experimental study of the 14N(p,γ)15O reaction at high and low energies
Abstract The 14 N ( p , γ ) 15 O reaction controls the rate of the carbon–nitrogen–oxygen (CNO) cycle of stellar hydrogen burning. The reaction proceeds by capture to the ground state and severalExpand
Radiative p14N Capture to the Third Excited State of the 15O Nucleus at 6.17 MeV
Within the framework of the modified potential cluster model, results of a description of available experimental data in terms of the astrophysical S-factor for the reaction of p14N capture to theExpand
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In the present work we report on a new measurement of resonance strengths ! in the reaction 25 Mg(p,) 26 Al at Ecm = 92 and 189 keV. This study was performed at the LUNA facility in the Gran SassoExpand
Direct measurements of low-energy resonance strengths of the 23Na(p,γ)24Mg reaction for astrophysics
Abstract The NeNa and the MgAl cycles play a fundamental role in the nucleosynthesis of asymptotic giant branch stars undergoing hot bottom burning. The Na 23 ( p , γ ) 24 Mg reaction links these twoExpand
First measurement of the 14N(p,γ)15O cross section down to 70 keV
Abstract In stars with temperatures above 20 × 10 6 K , hydrogen burning is dominated by the CNO cycle. Its rate is determined by the slowest process, the 14N(p, γ)15O reaction. Deep underground inExpand
Astrophysical implications of the proton-proton cross section updates
Abstract The p ( p , e + ν e ) H 2 reaction rate is an essential ingredient for theoretical computations of stellar models. In the past several values of the corresponding S -factor have been madeExpand
Radiative р14N Capture to the Second and Fifth Excited States of 15O
Within the framework of the modified potential cluster model, we have obtained a description of the available experimental data on the astrophysical S-factor of the p14N capture reaction to theExpand
Low-energy resonances in the O18 ( p,γ)19F reaction
Background: Shell hydrogen burning during the asymptotic giant branch (AGB) phase through the oxygen isotopes has been indicated as a key process that is needed to understand the observed O 18 / O 16Expand


Stellar reaction rate of 14N(p, γ)15O and hydrogen burning in massive stars☆
Abstract The capture reaction 14 N(p, γ) 15 O has been investigated in the energy range E p = 0.2 to 3.6 MeV with the use of windowless gas targets as well as implanted 14 N solid targets of highExpand
Direct measurement of the 14N(p,gamma)15O S factor.
The 14N(p,gamma)15O reaction regulates the rate of energy generation in the stellar CN cycle and is measured for energies in the range E(lab)(p)=155-524 keV, yielding a value for the S factor at zero energy which is significantly smaller than the previous result. Expand
The 14 N(p, γ ) 15 O low-energy S -factor
Abstract The 14N(p, γ )15O low-energy S -factor is analyzed using the R -matrix model. We find that the g.s. contribution is less than previously reported. The S -factor is mainly given by the 6.79Expand
Astrophysical S-factor of 14N( p, ?) 15O
We report on a new measurement of the 14N(p,γ) 15O capture cross section at Ep=140 to 400 keV using the 400 kV LUNA accelerator facility at the Laboratori Nazionali del Gran Sasso (LNGS). The uncerExpand
The 14N(p,γ)15O reaction, solar neutrinos and the age of the globular clusters
Abstract We discuss implications of a new measurement of 14 N (p,γ) 15 O concerning solar neutrinos, solar models and globular cluster dating. Predictions for the gallium and chlorine experiments areExpand
Lifetime of the 6793-keV state in 15O.
A mean lifetime of 1.60(+0.75)(-0.72) fs (90% C.L.) for this state using the Doppler-shift attenuation method implies that the contribution of the subthreshold resonance is negligible. Expand
E1 strength of the subthreshold 3/2+ state in 15O studied by Coulomb excitation
Abstract The radiative width of the 3/2 + state at 6.793 MeV in 15 O has been experimentally determined to be Γ γ =0.95 +0.60 −0.95  eV by intermediate-energy Coulomb excitation. Our resultExpand
Analyzing power measurement for the 14 N ( p→ ,γ) 15 O reaction at astrophysically relevant energies
S. O. Nelson, M. W. Ahmed, B. A. Perdue, K. Sabourov, A. L. Sabourov, A. P. Tonchev, R. M. Prior, M. Spraker, and H. R. Weller Department of Physics, Duke University, Durham, North Carolina 27708,Expand
Asymptotic normalization coefficients for 14 N ¿ p \ 15 O and the astrophysical S factor for 14 N „ p , g ... 15
The N(p,g)O reaction, which controls energy production in the CNO cycle, has contributions from both resonance and direct captures to the ground and excited states. The overall normalization of theExpand
A compilation of charged-particle induced thermonuclear reaction rates
Low-energy cross section data for 86 charged-particle induced reactions involving light (1 less than or equal to Z less than or equal to 14), mostly stable, nuclei are compiled. The correspondingExpand