First 80Se(n,γ) cross section measurement with high resolution in the full stellar energy range 1 eV - 100 keV and its astrophysical implications for the s-process

EPJ Web of Conferences

卷:260

¹  Mengoni A.²  Wallner A.³  Saxena A.⁴  Moreno-Soto J.⁵  Berthoumieux E.⁵  Dupont E.⁵  Gunsing F.⁵  Mendoza E.⁶  González-Romero E.⁶  Martínez T.⁶  Alcayne V.⁶  Cano-Ott D.⁶  Valenta S.⁷  Krtička M.⁷  Knapová I.⁷  Žugec P.⁸  Bosnar D.⁸  Rauscher T.⁹  Heyse J.¹⁰  Schillebeeckx P.¹⁰  Calviani M.¹¹  Bacak M.¹¹  Mastromarco M.¹¹  Masi A.¹¹  Rubbia C.¹¹  Macina D.¹¹  Kadi Y.¹¹  Barbagallo M.¹¹  Tsinganis A.¹¹  Mingrone F.¹¹  Vlachoudis V.¹¹  Gilardoni S.¹¹  Ferrari A.¹¹  Cerutti F.¹¹  Tassan-Got L.¹¹  Aberle O.¹¹  Chiaveri E.¹¹  Göbel K.¹²  Thomas Th.¹²  Kurtulgil D.¹²  Reifarth R.¹²  Urlass S.¹³  Junghans A.¹³  Oprea A.¹⁴  Petrone C.¹⁴  Negret A.¹⁴  Musumarra A.¹⁵  Finocchiaro P.¹⁵  Amaducci S.¹⁵  Cosentino L.¹⁵  Ramos-Doval D.¹⁶  Audouin L.¹⁶  Romanets Y.¹⁷  Gonçalves I. F.¹⁷  Vaz P.¹⁷  Domingo-Pardo C.¹⁸  Caballero-Ontanaya L.¹⁸  Ladarescu I.¹⁸  Balibrea-Correa J.¹⁸  Tain J. L.¹⁸  Babiano-Suarez V.¹⁸  Cristallo S.¹⁹  Damone L. A.¹⁹  Tagliente G.¹⁹  Variale V.¹⁹  Massimi C.¹⁹  Manna A.¹⁹  Mastinu P.¹⁹  Milazzo P. M.¹⁹  Busso M.¹⁹  Vannini G.¹⁹  Ventura A.¹⁹  Mazzone A.¹⁹  Persanti L.¹⁹  Colonna N.¹⁹  Vescovi D.¹⁹  Kimura A.²⁰  Harada H.²⁰  Furman V.²¹  Kopatch Y.²¹  Käppeler F.²²  Kokkoris M.²³  Stamatopoulos A.²³  Michalopoulou V.²³  Diakaki M.²³  Vlastou R.²³  Maugeri E. A.²⁴  Rochman D.²⁴  Heinitz S.²⁴  Sprung P.²⁴  Dressler R.²⁴  Ulrich J.²⁴  Schumann D.²⁴  Nolte R.²⁵  Pirovano E.²⁵  Ducasse Q.²⁵  Dietz M.²⁶  Lonsdale S. J.²⁶  Lederer-Woods C.²⁶  Garg R.²⁶  Woods P. J.²⁶  Leeb H.²⁷  Lerendegui-Marco J.²⁸  CortésGiraldo M. A.²⁸  Sabaté-Gilarte M.²⁸  Guerrero C.²⁸  Quesada J. M.²⁸  Cortés G.²⁹  Tarifeño-Saldivia A.²⁹  Calviño F.²⁹  Casanovas A.²⁹  Porras I.³⁰  Torres-Sánchez P.³⁰  Ogállar F.³⁰  Praena J.³⁰  Eleme Z.³¹  Patronis N.³¹  Gawlik-Ramięga A.³²  Perkowski J.³²  Andrzejewski J.³²  Smith A. G.³³  Sosnin N. V.³³  Bennett S.³³  Billowes J.³³  Sekhar A.³³  Wright T.³³  Davies P. J.³³  Durán I.³⁴  Caamaño M.³⁴  Fernández-Domínguez B.³⁴  Pavlik A.³⁵  Jenkins D. G.³⁶  Brown A.³⁶ 

[1] ;

[2] Agenzia nazionale per le nuove tecnologie (ENEA);

[3] Australian National University;

[4] Bhabha Atomic Research Centre (BARC);

[5] CEA Irfu, Universite Paris-Saclay;

[6] Centro de Investigaciones Energeticas Medioambientales y Tecnologicas (CIEMAT);

[7] Charles University;

[8] Department of Physics, Faculty of Science, University of Zagreb;

[9] Department of Physics, University of Basel;

[10] European Commission, Joint Research Centre (JRC);

[11] European Organization for Nuclear Research (CERN);

[12] Goethe University Frankfurt;

[13] Helmholtz-Zentrum Dresden-Rossendorf;

[14] Horia Hulubei National Institute of Physics and Nuclear Engineering;

[15] INFN Laboratori Nazionali del Sud;

[16] Institut de Physique Nucleaire, CNRS-IN2P3, Univ. Paris-Sud, Universite Paris-Saclay;

[17] Instituto Superior Tecnico;

[18] Instituto de Fisica Corpuscular, CSIC - Universidad de Valencia;

[19] Istituto Nazionale di Fisica Nucleare;

[20] Japan Atomic Energy Agency (JAEA);

[21] Joint Institute for Nuclear Research (JINR);

[22] Karlsruhe Institute of Technology, Campus North, IKP;

[23] National Technical University of Athens;

[24] Paul Scherrer Institut (PSI);

[25] Physikalisch-Technische Bundesanstalt (PTB);

[26] School of Physics and Astronomy, University of Edinburgh;

[27] TU Wien, Atominstitut;

[28] Universidad de Sevilla;

[29] Universitat Politecnica de Catalunya;

[30] University of Granada;

[31] University of Ioannina;

[32] University of Lodz;

[33] University of Manchester;

[34] University of Santiago de Compostela;

[35] University of Vienna, Faculty of Physics;

[36] University of York;

关键词: ;   

DOI  :  10.1051/epjconf/202226011026

来源: DOAJ

【 摘 要 】

Most elements heavier than iron have been generated in the stellar media by means of neutron capture reactions, approximately half are produced by the slow neutron capture or s-process. Radiative neutron capture cross section measurements are of fundamental importance for the study of this mechanism. In this contribution we present a brief summary on the measurement and results for the 80Se(n,γ) cross-section. The experiment was carried out at CERN n_TOF EAR1 via the time of flight (ToF) technique, using four C6D6 scintillation detectors with very fast response. More than a hundred new resonances have been analyzed for the first time with a high accuracy. The MACS obtained at kT = 8 keV is 36% smaller than the recommended value in KADo-NiS. Some of the astrophysical implications of this result are elucidated in this contribution.

【 授权许可】

Unknown