Measurement of the 78Se(n, γ) 79Se cross section up to 600 keV at the n_TOF facility at CERN

The 78Se(n, γ ) 79Se cross section has a high impact on the abundances of 78Se produced during the slow neutron capture process (s process) in massive stars. A measurement of the 78Se radiative neutron capture cross section has been performed at the Neutron Time-of-Flight facility at CERN using a set of liquid scintillation detectors that have been optimized for a low sensitivity to neutrons. We present resonance capture kernels up to 70 keV and cross section from 70 to 600 keV. Maxwellian-averaged cross section (MACS) values were calculated for stellar temperatures between kT = 5 and 100 keV, with uncertainties between 4.6% and 5.8%. The new MACS values result in substantial decreases of 20–30% of 78Se abundances produced in the s process in massive stars and AGB stars. Massive stars are now predicted to produce subsolar 78Se / 76Se ratios, which is expected since 76Se is an s-only isotope, while solar 78Se abundances have also contributions from other nucleosynthesis processes.

SOSNIN N. V.;  LEDERER-WOODS Claudia;  GARG R.;  BATTINO U.;  CRISTALLO S.;  DIETZ M.;  HEINITZ S.;  KRTICKA M.;  REIFARTH R.;  VALENTA S.;  VESCOVI D.;  ABERLE O.;  ALCAYNE V.;  AMADUCCI S.;  ANDRZEJEWSKI J.;  AUDOUIN L.;  BECARES V.;  BABIANO-SUAREZ V.;  BACAK M.;  BARBAGALLO M;  BECVAR F.;  BELLIA G.;  BERTHOUMIEUX E.;  BILLOWES J.;  BOSNAR D.;  BROWN A.;  BUSSO M.;  CAAMANO M.;  CABALLERO-ONTANAYA L.;  CALVINO F.;  CALVIANI M.;  CANO-OTT D.;  CASANOVAS A.;  CERUTTI F.;  CHEN Y. H.;  CHIAVERI E.;  COLONNA N.;  CORTÉS G. P.;  CORTES-GIRALDO M. A.;  COSENTINO Luigi;  DAMONE L.;  DIAKAKI M.;  DOMINGO-PARDO C.;  DRESSLER R.;  DUPONT E.;  DURAN I.;  ELEME Z.;  FERNÁNDEZ-DOMÍNGEZ B.;  FERRARI A.;  FINOCCHIARO Paolo;  FURMAN V.;  GÖBEL K.;  GAWLIK-RAMIEGA A.;  GILARDONI S.;  GLODARIU T.;  GONCALVES I. F.;  GONZÁLEZ-ROMERO E.;  GUERRERO C.;  GUNSING F.;  HARADA H.;  HEYSE Jan;  JENKINS D. G.;  JERICHA E.;  KAEPPELER F.;  KADI Y.;  KIMURA A.;  KIVEL N.;  KOKKORIS M.;  KOPATCH Y.;  KURTULGIL D.;  LADARESCU I.;  LEEB H.;  LERENDEGUI-MARCO J.;  LO MEO S.;  LONSDALE S.;  MANNA A;  MARTÍNEZ T.;  MASI A.;  MASSIMI C.;  MASTINU P.;  MASTROMARCO M.;  MATTEUCCI F.;  MAUGERI E.;  MAZZONE A.;  MENDOZA E.;  MENGONI A.;  MICHALOPOULOU V.;  MILAZZO P. M.;  MURPHY A. St. J.;  MUSUMARRA A.;  NEGRET A.;  NOLTE R.;  OGALLAR F.;  OPREA A.;  PATRONIS N.;  PAVLIK A.;  PERKOWSKI J.;  PIERSANTI L.;  PORRAS I.;  PRAENA J.;  QUESADA J.;  RADECK D.;  RAMOS-DOVAL D.;  RAUSCHER T.;  ROCHMAN Dimitri Alexandre;  RUBBIA C.;  SABATE-GILARTE M;  SAXENA A.;  SCHILLEBEECKX Peter;  SCHUMANN D.;  SMITH A. G.;  STAMATOPOULOS A.;  TAGLIENTE G.;  TAIN J. L.;  TALIP Z.;  TARIFENO-SALDIVIA A.;  TASSAN-GOT L.;  TORRES-SANCHEZ P.;  TSINGANIS A.;  ULRICH J.;  URLASS S.;  VANNINI G.;  VARIALE V.;  VAZ P.;  VENTURA A.;  VLACHOUDIS V.;  VLASTOU R.;  WALLNER A.;  WOODS P. J.;  WRIGHT T. J.;  ZUGEC P.; 

2025-07-30

AMER PHYSICAL SOC

JRC138878

2469-9993 (online),   

https://journals.aps.org/prc/abstract/10.1103/PhysRevC.110.065805,    https://publications.jrc.ec.europa.eu/repository/handle/JRC138878,   

10.1103/PhysRevC.110.065805 (online),