Constraining the S-factor for 15N(p,gamma)16O reaction at astrophysical energies
- P. J. Le Blanc
- G. Imbriani
- J. Gorres
- M. Junker
- R. Azuma
- M. Beard
- D. Bemmerer
- A. Best
- C. Broggini
- A. Caciolli
- P. Corvisiero
- H. Costantini
- M. Couder
- R. DeBoer
- Z. Elekes
- S. Falahat
- A. Formicola
- Zs. Fulop
- G. Gervino
- A. Guglielmetti
- C. Gustavino
- Gy. Gyurky
- F. Kappeler
- A. Kontos
- R. Kuntz
- H. Leiste
- A. Lemut
- Q. Li
- B. Limata
- M. Marta
- C. Mazzocchi
- R. Menegazzo
- S. O. Brien
- A. Palumbo
- P. Prati
- V. Roca
- C. Rolfs
- C. Rossi Alvarez
- E. Somorjai
- E. Stech
- O. Straniero
- F. Strieder
- W. Tan
- F. Terrasi
- H. P. Trautvetter
- E. Uberseder
- M. Wiescher
DOIAbstract
The 15N(p,\u3b3)16O reaction represents a breakout reaction linking the first and second cycles 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 and 1028 keV, and a direct capture contribution to the ground state of 16O. Interference effects between these contributions both in the low-energy region (Ep<338 keV) and between the two resonances (338<Ep<1028 keV) can dramatically affect the extrapolation to energies of astrophysical interest. To facilitate a reliable extrapolation, the 15N(p,\u3b3)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 mu...
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