and ( ,tot) measurements at the GELINA and n_TOF facilities

Tagliente, G.; Kopecky, S.; Heyse, J.; Krti??ka, M.; Massimi, C.; Mengoni, A.; Milazzo, P. M.; Plompen, A. J. M.; Schillebeeckx, P.; Valenta, S.; Wynants, R.; Altstadt, S.; Andrzejewski, J.; Audouin, L.; B??cares, V.; Barbagallo, M.; Be??v????, F.; Belloni, F.; Berthoumieux, E.; Billowes, J.; Boccone, V.; Bosnar, D.; Brugger, M.; Calvi??o, F.; Calviani, M.; Cano-Ott, D.; Carrapi??o, C.; Cerutti, F.; Chiaveri, E.; Chin, M.; Colonna, N.; Cort??s, G.; Cort??s-Giraldo, M. A.; Cristallo, S.; Diakaki, M.; Domingo-Pardo, C.; Dressler, R.; Dur??n, I.; Eleftheriadis, C.; Ferrari, A.; Fraval, K.; Furman, V.; G??bel, K.; G??mez-Hornillos, M. B.; Ganesan, S.; Garc??a, A. R.; Giubrone, G.; Gon??alves, I. F.; Gonz??lez-Romero, E.; Goverdovski, A.; Griesmayer, E.; Guerrero, C.; Gunsing, F.; Heftrich, T.; Hern??ndez-Prieto, A.; Jericha, E.; K??ppeler, F.; Kadi, Y.; Karadimos, D.; Katabuchi, T.; Ketlerov, V.; Khryachkov, V.; Kivel, N.; Kokkoris, M.; Kroll, J.; Lampoudis, C.; Langer, C.; Leal-Cidoncha, E.; Lederer, C.; Leeb, H.; Leong, L. S.; Losito, R.; Lugaro, M.; Mallick, A.; Manousos, A.; Marganiec, J.; Mart??nez, T.; Mastinu, P.; Mastromarco, M.; Mendoza, E.; Mingrone, F.; Mirea, M.; Paradela, C.; Pavlik, A.; Perkowski, J.; Praena, J.; Quesada, J. M.; Rauscher, T.; Reifarth, R.; Riego-Perez, A.; Robles, M.; Rubbia, C.; Ryan, J. A.; Sabat??-Gilarte, M.; Sarmento, R.; Saxena, A.; Schmidt, S.; Schumann, D.; Sedyshev, P.; Tain, J. L.; Tarife??o-Saldivia, A.; Tarr??o, D.; Tassan-Got, L.; Tsinganis, A.; Vannini, G.; Variale, V.; Vaz, P.; Ventura, A.; Vermeulen, M. J.; Vescovi, D.; Vlachoudis, V.; Vlastou, R.; Wallner, A.; Ware, T.; Weigand, M.; Weiss, C.; Wright, T.; ??ugec, P.

doi:10.1103/physrevc.105.025805

Background: Stellar nucleosynthesis of elements heavier than iron is driven by neutron capture processes. Zr-92 is positioned at a strategic point along the slow nucleosynthesis path, given its proximity to the neutron magic number N = 50 and its position at the matching region between the weak and main slow processes.Purpose: In parallel with recent improved astronomical data, the extraction of accurate Maxwellian averaged cross sections (MACSs) derived from a more complete and accurate set of resonance parameters should allow for a better understanding of the stellar conditions at which nucleosynthesis takes place.Methods: Transmission and capture cross section measurements using enriched Zr-92 metallic samples were performed at the time-of flight facilities GELINA of JRC-Geel (BE) and n_TOF of CERN (CH). The neutron beam passing through the samples was investigated in transmission measurements at GELINA using a Li-glass scintillator. The gamma rays emitted during the neutron capture reactions were detected by C6D6 detectors at both GELINA and n_TOF.Results: Resonance parameters of individual resonances up to 81 keV were extracted from a combined resonance shape analysis of experimental transmissions and capture yields. For the majority of the resonances the parity was determined from an analysis of the transmission data obtained with different sample thicknesses. Average resonance parameters were calculated.Conclusions: Maxwellian averaged cross sections were extracted from resonances observed up to 81 keV. The MACS for kT = 30 keV is fully consistent with experimental data reported in the literature. The MACSs for kT less than or similar to 15 keV are in good agreement with those derived from the ENDF/B-VIII.0 library and recommended in the KADoNTS database. For kT higher than 30 keV differences are observed. A comparison with MACSs obtained with the cross sections recommended in the JEFF-3.3 and JENDL-4.0 libraries shows discrepancies even for kT less than or similar to 15 keV.