{"paper":{"title":"$^{62}$Ni($n,\\gamma$) and $^{63}$Ni($n,\\gamma$) cross sections measured at n_TOF/CERN","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"nucl-ex","authors_text":"A. Ferrari, A. Manousos, A. Mengoni, A. Pavlik, A. Plompen, A.R. Garc{\\i}a, A. Riego, A. Tsinganis, A. Ventura, A. Wallner, B. Berthier, C. Carrapico, C. Domingo-Pardo, C. Eleftheriadis, C. Guerrero, C. Langer, C. Lederer, C. Massimi, C. Paradela, C. Rubbia, C. Wei{\\ss}, D. Bosnar, D. Cano-Ott, D.G. Jenkins, D. Karadimos, D. Schumann, D. Tarr{\\i}o, E. Berthoumieux, E. Chiaveri, E. Gonzalez-Romero, E. Griesmayer, E. Jericha, E. Lebbos, E. Mendoza, F. Becvar, F. Belloni, F. Calvino, F. Cerutti, F. Gramegna, F. Gunsing, F. K\\\"appeler, F. Mingrone, F. Roman, G. Cortes, G. Giubrone, G. Korschinek, G. Tagliente, G. Vannini, H. Leeb, I. Dillmann, I. Duran, I.F. Goncalves, J. Andrzejewski, J. Billowes, J. Kroll, J.L. Tain, J. Marganiec, J.M. Quesada, J. Perkowski, J. Praena, K. Fraval, K. Ioannides, L. Audouin, L.S. Leong, L. Tassan-Got, L. Tlustos, M.A. Cortes-Giraldo, M. Barbagallo, M.B. Gomez-Hornillos, M. Brugger, M. Calviani, M. Chin, M. Fernandez-Ordonez, M. Heil, M.J. Vermeulen, M. Krticka, M. Lozano, M. Mastromarco, M. Meaze, M. Mirea, M. Pignatari, M. Weigand, N. Colonna, N. Dzysiuk, N. Kivel, P.F. Mastinu, P. Gurusamy, P.M. Milazzo, P. Schillebeeckx, P. Vaz, P. Zugec, R. Dressler, R. Losito, R. Plag, R. Reifarth, R. Sarmento, R. Versaci, R. Vlastou, S. Altstadt, S. Andriamonje, S. Ganesan, S. Harrisopulos, S. Marrone, S. Schmidt, S. Valenta, T.J. Wright, T. Martinez, T. Rauscher, T. Ware, V. Becares, V. Boccone, V. Variale, V. Vlachoudis, W. Mondalaers, Y. Kadi","submitted_at":"2014-03-19T12:03:21Z","abstract_excerpt":"The cross section of the $^{62}$Ni($n,\\gamma$) 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 $^{63}$Ni($n,\\gamma$) reaction was me"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1403.4778","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}