Experimental neutron capture data of 58Ni from the CERN n_TOF facility
- Zugec, P.
- Barbagallo, M.
- Colonna, N.
- Bosnar, D.
- Altstadt, S.
- Andrzejewski, J.
- Audouin, L.
- Bécares, V.
- Bev cváv r, F.
- Belloni, F.
- Berthoumieux, E.
- Billowes, J.
- Boccone, V.
- Brugger, M.
- Calviani, M.
- Calviño, F.
- Cano-Ott, D.
- Carrapic co, C.
- Cerutti, F.
- Chiaveri, E.
- Chin, M.
- Cortés, G.
- Cortés-Giraldo, M. A.
- Diakaki, M.
- Domingo-Pardo, C.
- Dressler, R.
- Duran, I.
- Dzysiuk, N.
- Eleftheriadis, C.
- Ferrari, A.
- Fraval, K.
- Ganesan, S.
- Garc`ia, A. R.
- Giubrone, G.
- Gómez-Hornillos, M. B.
- Gonc calves, I. F.
- González-Romero, E.
- Griesmayer, E.
- Guerrero, C.
- Gunsing, F.
- Gurusamy, P.
- Heinitz, S.
- Jenkins, D. G.
- Jericha, E.
- Kadi, Y.
- Käppeler, F.
- Karadimos, D.
- Kivel, N.
- Koehler, P.
- Kokkoris, M.
- Krtiv cka, M.
- Kroll, J.
- Langer, C.
- Lederer, C.
- Leeb, H.
- Leong, L. S.
- Lo Meo, S.
- Losito, R.
- Manousos, A.
- Marganiec, J.
- Mart`inez, T.
- Massimi, C.
- Mastinu, P. F.
- Mastromarco, M.
- Meaze, M.
- Mendoza, E.
- Mengoni, A.
- Milazzo, P. M.
- Mingrone, F.
- Mirea, M.
- Mondalaers, W.
- Paradela, C.
- Pavlik, A.
- Perkowski, J.
- Pignatari, M.
- Plompen, A.
- Praena, J.
- Quesada, J. M.
- Rauscher, T.
- Reifarth, R.
- Riegov, A.
- Roman, F.
- Rubbia, C.
- Sarmento, R.
- Saxena, A.
- Schillebeeckx, P.
- Schmidt, S.
- Schumann, D.
- Tagliente, G.
- Tain, J. L.
- Tarr`io, D.
- Tassan-Got, L.
- Tsinganis, A.
- Valenta, S.
- Vannini, G.
- Variale, V.
- Vaz, P.
- Ventura, A.
- Versaci, R.
- Vermeulen, M. J.
- Vlachoudis, V.
- Vlastou, R.
- Wallner, A.
- Ware, T.
- Weigand, M.
- Weiß, C.
- Wright, T.
DOIAbstract
The neutron capture cross section of 58Ni was measured at the neutron time of flight facility n_TOF at CERN, from 27 meV to 400 keV neutron energy. Special care has been taken to identify all the possible sources of background, with the so-called neutron background obtained for the first time using high-precision GEANT4 simulations. The energy range up to 122 keV was treated as the resolved resonance region, where 51 resonances were identified and analyzed by a multilevel R-matrix code SAMMY. Above 122 keV the code SESH was used in analyzing the unresolved resonance region of the capture yield. Maxwellian averaged cross sections were calculated in the temperature range of kT = 5 – 100 keV, and their astrophysical implications were investiga...
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