Cross section of the reaction 18O(p,γ)19F at astrophysical energies: The 90 keV resonance and the direct capture component
Autor: | Rosanna Depalo, A. Best, Maria Lugaro, A. Formicola, Paolo Prati, Gianluca Imbriani, G. Gervino, A. Di Leva, A. Guglielmetti, László Csedreki, F. Ferraro, Carlo Broggini, Z. Elekes, K. Stöckel, R. Perrino, I. Kochanek, E. M. Fiore, T. Chillery, Roberto Menegazzo, Davide Trezzi, A. Boeltzig, P. Corvisiero, Raffaele Buompane, Sandra Zavatarelli, Thomas Davinson, Gy. Gyürky, Paola Marigo, Daniel Bemmerer, C. Gustavino, M. Junker, Frank Strieder, F. Cavanna, Michael Wiescher, D. Piatti, Tamás Szücs, C. G. Bruno, Richard deBoer, V. Paticchio, F. R. Pantaleo, Oscar Straniero, Marialuisa Aliotta, L. Schiavulli, M. P. Takács, G. F. Ciani, Antonio Caciolli, V. Mossa, Zs. Fülöp, J. Balibrea-Correa |
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Přispěvatelé: | Best, A., Pantaleo, F. R., Boeltzig, A., Imbriani, G., Aliotta, M., Balibrea-Correa, J., Bemmerer, D., Broggini, C., Bruno, C. G., Buompane, R., Caciolli, A., Cavanna, F., Chillery, T., Ciani, G. F., Corvisiero, P., Csedreki, L., Davinson, T., Deboer, R. J., Depalo, R., Di Leva, A., Elekes, Z., Ferraro, F., Fiore, E. M., Formicola, A., Fulop, Z., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, G., Junker, M., Kochanek, I., Lugaro, M., Marigo, P., Menegazzo, R., Mossa, V., Paticchio, V., Perrino, R., Piatti, D., Prati, P., Schiavulli, L., Stockel, K., Straniero, O., Strieder, F., Szucs, T., Takacs, M. P., Trezzi, D., Wiescher, M., Zavatarelli, S. |
Jazyk: | angličtina |
Rok vydání: | 2019 |
Předmět: |
Nuclear reaction
Nuclear and High Energy Physics Experimental nuclear astrophysics 01 natural sciences Resonance (particle physics) Isotopes of oxygen Stellar evolution Reaction rate Nuclear physics Cross section (physics) Hydrogen burning Underground nuclear physics 0103 physical sciences Experimental nuclear astrophysics Underground nuclear physics Hydrogen burning Stellar evolution Nuclear astrophysics 010306 general physics Nuclear Experiment Physics Experimental nuclear astrophysic 010308 nuclear & particles physics Giant star lcsh:QC1-999 Orders of magnitude (time) lcsh:Physics |
Zdroj: | Physics Letters B, Vol 797, Iss, Pp-(2019) Best, A, Pantaleo, F R, Boeltzig, A, Imbriani, G, Aliotta, M, Balibrea-Correa, J, Bemmerer, D, Broggini, C, Bruno, C G, Buompane, R, Caciolli, A, Cavanna, F, Chillery, T, Ciani, G F, Corvisiero, P, Csedreki, L, Davinson, T, deBoer, R J, Depalo, R, Di Leva, A, Elekes, Z, Ferraro, F, Fiore, E M, Formicola, A, Fülöp, Z, Gervino, G, Guglielmetti, A, Gustavino, C, Gyürky, G, Junker, M, Kochanek, I, Lugaro, M, Marigo, P, Menegazzo, R, Mossa, V, Paticchio, V, Perrino, R, Piatti, D, Prati, P, Schiavulli, L, Stöckel, K, Straniero, O, Strieder, F, Szücs, T, Takács, M P, Trezzi, D, Wiescher, M & Zavatarelli, S 2019, ' Cross section of the reaction 18O(p,γ)19F at astrophysical energies: The 90 keV resonance and the direct capture component ', Physics Letters B, vol. 797, 134900 . https://doi.org/10.1016/j.physletb.2019.134900 Physics Letters B 797(2019), 134900 |
ISSN: | 0370-2693 |
Popis: | The observation of oxygen isotopes in giant stars sheds light on mixing processes operating in their interiors. Due to the very strong correlation between nuclear burning and mixing processes it is very important to reduce the uncertainty on the cross sections of the nuclear reactions that are involved. In this paper we focus our attention on the reaction O 18 ( p , γ ) 19 F . While the O 18 ( p , α ) 15 N channel is thought to be dominant, the (p,γ) channel can still be an important component in stellar burning in giants, depending on the low energy cross section. So far only extrapolations from higher-energy measurements exist and recent estimates vary by orders of magnitude. These large uncertainties call for an experimental reinvestigation of this reaction. We present a direct measurement of the O 18 ( p , γ ) 19 F cross section using a high-efficiency 4π BGO summing detector at the Laboratory for Underground Nuclear Astrophysics (LUNA). The reaction cross section has been directly determined for the first time from 140 keV down to 85 keV and the different cross section components have been obtained individually. The previously highly uncertain strength of the 90 keV resonance was found to be 0.53 ± 0.07 neV, three orders of magnitude lower than an indirect estimate based on nuclear properties of the resonant state and a factor of 20 lower than a recently established upper limit, excluding the possibility that the 90 keV resonance can contribute significantly to the stellar reaction rate. |
Databáze: | OpenAIRE |
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