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

The cross section of the 62Ni(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 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 63Ni(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.

LEDERER C.;  MASSIMI C.;  BERTHOUMIEUX E.;  COLONNA N.;  DRESSLER R.;  GUERRERO C.;  GUNSING F.;  KÄPPELER F.;  KIVEL Niko;  PIGNATARI M.;  REIFARTH R.;  SCHUMANN D.;  WALLNER A.;  ANDRIAMONJE S.;  ANDRZEJEWSKI J.;  AUDOUIN L.;  BECVÁR F.;  CALVINO F.;  CANO-OTT D.;  CORTES G.;  DOMINGO-PARDO C.;  DURAN I.;  ELEFTHERIADIS C.;  FERRARI A.;  GONCALVES I.;  GONZALEZ-ROMERO E.;  GRIESMAYER E.;  JERICHA E.;  KADI Y.;  KARADIMOS D.;  KRTICKA M.;  LEEB H.;  MARGANIEC J.;  MASTINU P.;  MENGONI A.;  MILAZZO P. M.;  PARADELA C.;  PAVLIK A.;  PLOMPEN Arjan;  QUESADA J.;  RAUSCHER T.;  RUBBIA C.;  TAGLIENTE G.;  TAIN J. L.;  TASSAN-GOT L.;  VANNINI G.;  VAZ P.;  VENTURA A.;  VLASTOU R.;  BECARES V.;  BILLOWES J.;  BOCCONE V.;  BOSNAR D.;  BRUGGER M.;  CARRAPICO C.;  CERUTTI F.;  CHIN M.;  CORTES-GIRALDO M. A.;  DZYSIUK N.;  FRAVAL K.;  GARCIA A. R.;  GIUBRONE G.;  GOMEZ-HORNILLOS M. B.;  JENKINS D. G.;  TARRIO D.;  VALENTA S.;  VARIALE V.;  VERSACI R.;  VERMEULEN M.;  WARE T.;  WEIGAND M.;  WRIGHT T. J.;  ZUGEC P.;  BARBAGALLO M.;  ALTSTADT S.;  BELLONI F.;  BERTHIER B.;  CALVIANI M.;  CHIAVERI E.;  LANGER C.;  LEONG L. S.;  LOSITO R.;  GANESAN S.;  MANOUSOS A;  MARTINEZ T.;  MASTROMARCO M.;  MEAZE M.;  MENDOZA E.;  MINGRONE F.;  MIREA M.;  MONDELAERS Willy;  PERKOWSKI J.;  PRAENA J.;  RIEGO A.;  ROMAN F.;  SARMENTO R.;  SCHILLEBEECKX Peter;  SCHMIDT S.;  DILLMANN I;  FERNANDEZ-ORDONEZ M.;  GRAMEGNA F.;  HARRISOPULOS S.;  HEIL M.;  IOANNIDES K.;  KORSCHINEK G.;  LEBBOS E.;  LOZANO M.;  MARRONE S.;  PLAG R.;  TSINGANIS A.;  TLUSTOS L.;  VLACHOUDIS V.;  WEISS C.;  KROLL J.;  GURUSAMY P.; 

2014-05-02

AMER PHYSICAL SOC

JRC87297

0556-2813,   

http://link.aps.org/doi/10.1103/PhysRevC.89.025810,    http://dx.doi.org/10.1103/PhysRevC.89.025810,    https://publications.jrc.ec.europa.eu/repository/handle/JRC87297,   

10.1103/PhysRevC.89.025810,