Measurement of the 77Se(n, & gamma;) cross section up to 200 keV at the n_TOF facility at CERN
N. V. Sosnin,C. Lederer-Woods,M. Krticka,R. Garg,M. Dietz,M. Bacak,M. Barbagallo,U. Battino,S. Cristallo,L. A. Damone,M. Diakaki,S. Heinitz,D. Macina,M. Mastromarco,F. Mingrone,A. St. J. Murphy,G. Tagliente,S. Valenta,D. Vescovi,O. Aberle,V. Alcayne,S. Amaducci,J. Andrzejewski,L. Audouin,V. Becares,V. Babiano-Suarez,F. Becvar,G. Bellia,E. Berthoumieux,J. Billowes,D. Bosnar,A. Brown,M. Busso,M. Caamano,L. Caballero,F. Calvino,M. Calviani,D. Cano-Ott,A. Casanovas,F. Cerutti,Y. H. Chen,E. Chiaveri,N. Colonna,G. Cortes,M. A. Cortes-Giraldo,L. Cosentino,C. Domingo-Pardo,R. Dressler,E. Dupont,I. Duran,Z. Eleme,B. Fernandez-Dominguez,A. Ferrari,P. Finocchiaro,K. Goebel,A. Gawlik-Ramiega,S. Gilardoni,T. Glodariu,I. F. Goncalves,E. Gonzalez-Romero,C. Guerrero,F. Gunsing,H. Harada,J. Heyse,D. G. Jenkins,E. Jericha,F. Kaeppeler,Y. Kadi,A. Kimura,N. Kivel,M. Kokkoris,D. Kurtulgil,I. Ladarescu,H. Leeb,J. Lerendegui-Marco,S. Lo Meo,S. Lonsdale,A. Manna,T. Martinez,A. Masi,C. Massimi,P. Mastinu,F. Matteucci,E. A. Maugeri,A. Mazzone,E. Mendoza,A. Mengoni,V. Michalopoulou,P. M. Milazzo,A. Musumarra,A. Negret,R. Nolte,F. Ogallar,A. Oprea,N. Patronis,A. Pavlik,J. Perkowski,L. Piersanti,I. Porras,J. Praena,J. M. Quesada,D. Radeck,D. Ramos-Doval,T. Rauscher,R. Reifarth,D. Rochman,C. Rubbia,M. Sabate-Gilarte,A. Saxena,P. Schillebeeckx,D. Schumann,A. G. Smith,A. Stamatopoulos,J. L. Tain,T. Talip,A. Tarifeno-Saldivia,L. Tassan-Got,P. Torres-Sanchez,A. Tsinganis,J. Ulrich,S. Urlass,G. Vannini,V. Variale,P. Vaz,A. Ventura,V. Vlachoudis,R. Vlastou,A. Wallner,P. J. Woods,T. Wright,P. Zugec
PHYSICAL REVIEW C（2023）
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摘要
The 77Se(n, & gamma;) reaction is of importance for 77Se abundance during the slow neutron capture process in massive stars. We have performed a new measurement of the 77Se radiative neutron capture cross section at the Neutron Time-of-Flight facility at CERN. Resonance capture kernels were derived up to 51 keV and cross sections up to 200 keV. Maxwellian-averaged cross sections were calculated for stellar temperatures between kT = 5 keV and kT = 100 keV, with uncertainties between 4.2% and 5.7%. Our results lead to substantial decreases of 14% and 19% in 77Se abundances produced through the slow neutron capture process in selected stellar models of 15M0 and 2M0, respectively, compared to using previous recommendation of the cross section.
