Ni-62(n,gamma) and Ni-63(n,gamma) cross sections measured at the n_TOF facility at CERN

C. Lederer, C. Massimi, E. Berthoumieux, N. Colonna, R. Dressler, C. Guerrero, F. Gunsing, F. Käppeler, N. Kivel, M. Pignatari, R. Reifarth, D. Schumann, A. Wallner, S. Altstadt, S. Andriamonje, J. Andrzejewski, L. Audouin, M. Barbagallo, V. Becares, F. BecvarF. Belloni, B. Berthier, J. Billowes, V. Boccone, D. Bosnar, M. Brugger, M. Calviani, F. Calvino, D. Cano-Ott, C. Carrapico, F. Cerutti, E. Chiaveri, M. Chin, G. Cortes, M. A. Cortes-Giraldo, I. Dillmann, C. Domingo-Pardo, I. Duran, N. Dzysiuk, C. Eleftheriadis, M. Fernandez-Ordonez, A. Ferrari, K. Fraval, S. Ganesan, A. R. Garcıa, G. Giubrone, M. B. Gomez-Hornillos, I. F. Goncalves, E. Gonzalez-Romero, F. Gramegna, E. Griesmayer, P. Gurusamy, S. Harrisopulos, M. Heil, K. Ioannides, D. G. Jenkins, E. Jericha, Y. Kadi, D. Karadimos, G. Korschinek, M. Krticka, J. Kroll, C. Langer, E. Lebbos, H. Leeb, L. S. Leong, R. Losito, M. Lozano, A. Manousos, J. Marganiec, S. Marrone, T. Martinez, P. F. Mastinu, M. Mastromarco, M. Meaze, E. Mendoza, A. Mengoni, P. M. Milazzo, F. Mingrone, M. Mirea, W. Mondalaers, C. Paradela, A. Pavlik, J. Perkowski, R. Plag, A. Plompen, J. Praena, J. M. Quesada, T. Rauscher, A. Riego, F. Roman, C. Rubbia, R. Sarmento, P. Schillebeeckx, S. Schmidt, G. Tagliente, J. L. Tain, D. Tarrıo, L. Tassan-Got, A. Tsinganis, L. Tlustos, S. Valenta, G. Vannini, V. Variale, P. Vaz, A. Ventura, M. J. Vermeulen, R. Versaci, V. Vlachoudis, R. Vlastou, T. Ware, M. Weigand, C. Weiß, T. J. Wright, P. Zugec

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The cross section of the Ni-62(n,gamma) reaction was measured with the time-of-flight technique at the neutron time-of-flight facility n_TOF at CERN. Capture kernels of 42 resonances were analyzed up to 200 keV neutron energy and Maxwellian averaged cross sections (MACS) from kT = 5-100 keV were calculated. With a total uncertainty of 4.5%, the stellar cross section is in excellent agreement with the the KADoNiS compilation at kT = 30 keV, while being systematically lower up to a factor of 1.6 at higher stellar temperatures. The cross section of the Ni-63(n,gamma) reaction was measured for the first time at n_TOF. We determined unresolved cross sections from 10 to 270 keV with a systematic uncertainty of 17%. These results provide fundamental constraints on s-process production of heavier species, especially the production of Cu in massive stars, which serve as the dominant source of Cu in the solar system.
Original languageEnglish
Article number025810
JournalPhysical Review C
Issue number2
Publication statusPublished - 28 Feb 2014


  • nucl-ex

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