In stars, four hydrogen nuclei are converted into a helium nucleus by two competing nuclear fusion processes: the proton - proton chain (p-p) and the carbon - nitrogen - oxygen (CNO) cycle. At temperatures higher than 2*107 K, the CNO cycle dominates the energy production. In particular, its rate is determined by the slowest reaction: 14N(p, gamma )15O. Direct measurement in a laboratory at the surface of the Earth is hampered by the background due to the cosmic rays. Here we report on an experiment performed with the LUNA (Laboratory for Underground Nuclear Astrophysics) accelerator placed deep underground in the INFN Gran Sasso laboratory (Italy). Thanks to the cosmic ray suppression provided by the mountain shield, we could measure the 14N(p, gamma )15O cross section for the first time directly at energies corresponding to stellar temperatures and with unprecedented accuracy. In particular we used a large solid angle BGO detector with a differentially pumped windowless gas target. The lowest measured energy is 70.1 keV. Our results have important consequences for the formation of carbon stars, for an independent lower limit on the age of the universe, and for solar neutrino flux.
Low energy underground study of 14N(p,gamma)15O cross section / A. Lemut, F. Confortola, D. Bemmerer, R. Bonetti, C. Broggini, P. Corvisiero, H. Costantini, J. Cruz, A. Formicola, Z.S. Fulop, G. Gervino, A. Guglielmetti, C. Gustavino, G. Gyurky, G. Imbriani, A.P. Jesus, M. Junker, B. Limata, R.M.P. Prati, V. Roca, C. Rolfs, D. Rogalla, M. Romano, C. Rossi Alvarez, F. Schumann, E. Somorjai, O. Straniero, F. Strieder, F. Terrasi, H.P. Trautvetter. - 831:(2006), pp. 383-387. [10.1063/1.2200958]
Low energy underground study of 14N(p,gamma)15O cross section
R. Bonetti;A. Guglielmetti;
2006
Abstract
In stars, four hydrogen nuclei are converted into a helium nucleus by two competing nuclear fusion processes: the proton - proton chain (p-p) and the carbon - nitrogen - oxygen (CNO) cycle. At temperatures higher than 2*107 K, the CNO cycle dominates the energy production. In particular, its rate is determined by the slowest reaction: 14N(p, gamma )15O. Direct measurement in a laboratory at the surface of the Earth is hampered by the background due to the cosmic rays. Here we report on an experiment performed with the LUNA (Laboratory for Underground Nuclear Astrophysics) accelerator placed deep underground in the INFN Gran Sasso laboratory (Italy). Thanks to the cosmic ray suppression provided by the mountain shield, we could measure the 14N(p, gamma )15O cross section for the first time directly at energies corresponding to stellar temperatures and with unprecedented accuracy. In particular we used a large solid angle BGO detector with a differentially pumped windowless gas target. The lowest measured energy is 70.1 keV. Our results have important consequences for the formation of carbon stars, for an independent lower limit on the age of the universe, and for solar neutrino flux.
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