%0 Journal Article %T $^{62}$Ni($n,¦Ã$) and $^{63}$Ni($n,¦Ã$) cross sections measured at n_TOF/CERN %A C. Lederer %A C. Massimi %A E. Berthoumieux %A N. Colonna %A R. Dressler %A C. Guerrero %A F. Gunsing %A F. K£¿ppeler %A N. Kivel %A M. Pignatari %A R. Reifarth %A D. Schumann %A A. Wallner %A S. Altstadt %A S. Andriamonje %A J. Andrzejewski %A L. Audouin %A M. Barbagallo %A V. Becares %A F. Becvar %A F. Belloni %A B. Berthier %A J. Billowes %A V. Boccone %A D. Bosnar %A M. Brugger %A M. Calviani %A F. Calvino %A D. Cano-Ott %A C. Carrapico %A F. Cerutti %A E. Chiaveri %A M. Chin %A G. Cortes %A M. A. Cortes-Giraldo %A I. Dillmann %A C. Domingo-Pardo %A I. Duran %A N. Dzysiuk %A C. Eleftheriadis %A M. Fernandez-Ordonez %A A. Ferrari %A K. Fraval %A S. Ganesan %A A. R. Garc£¿a %A G. Giubrone %A M. B. Gomez-Hornillos %A I. F. Goncalves %A E. Gonzalez-Romero %A F. Gramegna %A E. Griesmayer %A P. Gurusamy %A S. Harrisopulos %A M. Heil %A K. Ioannides %A D. G. Jenkins %A E. Jericha %A Y. Kadi %A D. Karadimos %A G. Korschinek %A M. Krticka %A J. Kroll %A C. Langer %A E. Lebbos %A H. Leeb %A L. S. Leong %A R. Losito %A M. Lozano %A A. Manousos %A J. Marganiec %A S. Marrone %A T. Martinez %A P. F. Mastinu %A M. Mastromarco %A M. Meaze %A E. Mendoza %A A. Mengoni %A P. M. Milazzo %A F. Mingrone %A M. Mirea %A W. Mondalaers %A C. Paradela %A A. Pavlik %A J. Perkowski %A R. Plag %A A. Plompen %A J. Praena %A J. M. Quesada %A T. Rauscher %A A. Riego %A F. Roman %A C. Rubbia %A R. Sarmento %A P. Schillebeeckx %A S. Schmidt %A G. Tagliente %A J. L. Tain %A D. Tarr£¿o %A L. Tassan-Got %A A. Tsinganis %A L. Tlustos %A S. Valenta %A G. Vannini %A V. Variale %A P. Vaz %A A. Ventura %A M. J. Vermeulen %A R. Versaci %A V. Vlachoudis %A R. Vlastou %A T. Ware %A M. Weigand %A C. Wei£¿ %A T. J. Wright %A P. Zugec %J Physics %D 2014 %I arXiv %R 10.1103/PhysRevC.89.025810 %X 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 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. %U http://arxiv.org/abs/1403.4778v1