Amaducci S. , Colonna N. , Cosentino L. , Cristallo S. , Finocchiaro P. , Krticka M. , Massimi C. , Mastromarco M. , Mazzone A. , Maugeri E.A. , Mengoni A. , Roederer I.U. , Straniero O. , Valenta S. , Vescovi D. , Aberle O. , Alcayne V. , Andrzejewski J. , Audouin L. , Babiano-Suarez V. , Bacak M. , Barbagallo M. , Bennett S. , Berthoumieux E. , Billowes J. , Bosnar D. , Brown A. , Busso M. , Caamaño M. , Caballero-Ontanaya L. , Calviño F. , Calviani M. , Cano-Ott D. , Casanovas A. , Cerutti F. , Chiaveri E. , Cortés G. , Cortés-Giraldo M.A. , Damone L.A. , Davies P.J. , Diakaki M. , Dietz M. , Domingo-Pardo C. , Dressler R. , Ducasse Q. , Dupont E. , Durán I. , Eleme Z. , Fernández-Domínguez B. , Ferrari A. , Furman V. , Göbel K. , Garg R. , Gawlik-Rami?ga A. , Gilardoni S. , Gonçalves I.F. , González-Romero E. , Guerrero C. , Gunsing F. , Harada H. , Heinitz S. , Heyse J. , Jenkins D.G. , Junghans A. , Käppeler F. , Kadi Y. , Kimura A. , Knapová I. , Kokkoris M. , Kopatch Y. , Kurtulgil D. , Ladarescu I. , Lederer-Woods C. , Leeb H. , Lerendegui-Marco J. , Lonsdale S.J. , Macina D. , Manna A. , Martínez T. , Masi A. , Mastinu P. , Mendoza E. , Michalopoulou V. , Milazzo P.M. , Mingrone F. , MORENO SOTO, JAVIER, Musumarra A. , Negret A. , Nolte R. , Ogállar F. , Oprea A. , Patronis N. , Pavlik A. , Perkowski J. , Petrone C. , Piersanti L. , Pirovano E. , Porras I. , Praena J. , Quesada J.M. , Ramos-Doval D. , Rauscher T. , Reifarth R. , Rochman D. , Rubbia C. , Sabaté-Gilarte M. , Saxena A. , Schillebeeckx P. , Schumann D. , Sekhar A. , Smith A.G. , Sosnin N.V. , Sprung P. , Stamatopoulos A. , Tagliente G. , Tain J.L. , Tarifeño-Saldivia A. , Tassan-Got L. , Thomas T. , Torres-Sánchez 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. , Žugec P.
No
Phys Rev Lett
Article
Científica
21/03/2024
2-s2.0-85188670848
Ce140(n,?) is a key reaction for slow neutron-capture (s-process) nucleosynthesis due to being a bottleneck in the reaction flow. For this reason, it was measured with high accuracy (uncertainty ˜5%) at the n_TOF facility, with an unprecedented combination of a high purity sample and low neutron-sensitivity detectors. The measured Maxwellian averaged cross section is up to 40% higher than previously accepted values. Stellar model calculations indicate a reduction around 20% of the s-process contribution to the Galactic cerium abundance and smaller sizeable differences for most of the heavier elements. No variations are found in the nucleosynthesis from massive stars. © 2024 authors. Published by the American Physical Society. Published by the American Physical Society under the terms of the "https://creativecommons.org/licenses/by/4.0/"Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI.
Chemical elements; Nucleosynthesis; cerium; Astrophysical implications; Chemical evolution; High-accuracy; Key reactions; Measurements of; Neutron capture; Reaction flow; S-process; Slow neutrons; Uncertainty; article; cosmos; evolution; neutron capture therapy; Atomic physics