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First $^{80}$Se(n,$\gamma$) cross section measurement with high resolution in the full stellar energy range 1 eV - 100 keV and its astrophysical implications for the s-process
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...
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| Lenguaje: | eng |
| Publicado: |
2022
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| Materias: | |
| Acceso en línea: | https://dx.doi.org/10.1051/epjconf/202226011026 http://cds.cern.ch/record/2861329 |
| _version_ | 1780977816629673984 |
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| author | Babiano-Suarez, V Balibrea-Correa, J Caballero-Ontanaya, L Domingo-Pardo, C Ladarescu, I Lerendegui-Marco, J Tain, J L Calviño, F Casanovas, A Tarifeño-Saldivia, A Guerrero, C Aberle, O Alcayne, V Amaducci, S Andrzejewski, J Audouin, L Bacak, M Barbagallo, M Bennett, S Berthoumieux, E Billowes, J Bosnar, D Brown, A Busso, M Caamaño, M Calviani, M Cano-Ott, D Cerutti, F Chiaveri, E Colonna, N Cortés, G CortésGiraldo, M A Cosentino, L Cristallo, S Damone, L A Davies, P J Diakaki, M Dietz, M Dressler, R Ducasse, Q Dupont, E Durán, I Eleme, Z Fernández-Domínguez, B Ferrari, A Finocchiaro, P Furman, V Göbel, K Garg, R Gawlik-Ramięga, A Gilardoni, S Gonçalves, I F González-Romero, E 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 Krtička, M Kurtulgil, D Lederer-Woods, C Leeb, H Lonsdale, S J Macina, D Manna, A Martínez, T Masi, A Massimi, C Mastinu, P Mastromarco, M Maugeri, E A Mazzone, A Mendoza, E Mengoni, A Michalopoulou, V Milazzo, P M Mingrone, F Moreno-Soto, J Musumarra, A Negret, A Nolte, R Ogállar, F Oprea, A Patronis, N Pavlik, A Perkowski, J Persanti, L Petrone, C Pirovano, E Porras, I Praena, J Quesada, J M Ramos-Doval, D Rauscher, T Reifarth, R Rochman, D Romanets, Y 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 Tassan-Got, L Thomas, Th Torres-Sánchez, P Tsinganis, A Ulrich, J Urlass, S Valenta, S Vannini, G Variale, V Vaz, P Ventura, A Vescovi, D Vlachoudis, V Vlastou, R Wallner, A Woods, P J Wright, T Žugec, P |
| author_facet | Babiano-Suarez, V Balibrea-Correa, J Caballero-Ontanaya, L Domingo-Pardo, C Ladarescu, I Lerendegui-Marco, J Tain, J L Calviño, F Casanovas, A Tarifeño-Saldivia, A Guerrero, C Aberle, O Alcayne, V Amaducci, S Andrzejewski, J Audouin, L Bacak, M Barbagallo, M Bennett, S Berthoumieux, E Billowes, J Bosnar, D Brown, A Busso, M Caamaño, M Calviani, M Cano-Ott, D Cerutti, F Chiaveri, E Colonna, N Cortés, G CortésGiraldo, M A Cosentino, L Cristallo, S Damone, L A Davies, P J Diakaki, M Dietz, M Dressler, R Ducasse, Q Dupont, E Durán, I Eleme, Z Fernández-Domínguez, B Ferrari, A Finocchiaro, P Furman, V Göbel, K Garg, R Gawlik-Ramięga, A Gilardoni, S Gonçalves, I F González-Romero, E 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 Krtička, M Kurtulgil, D Lederer-Woods, C Leeb, H Lonsdale, S J Macina, D Manna, A Martínez, T Masi, A Massimi, C Mastinu, P Mastromarco, M Maugeri, E A Mazzone, A Mendoza, E Mengoni, A Michalopoulou, V Milazzo, P M Mingrone, F Moreno-Soto, J Musumarra, A Negret, A Nolte, R Ogállar, F Oprea, A Patronis, N Pavlik, A Perkowski, J Persanti, L Petrone, C Pirovano, E Porras, I Praena, J Quesada, J M Ramos-Doval, D Rauscher, T Reifarth, R Rochman, D Romanets, Y 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 Tassan-Got, L Thomas, Th Torres-Sánchez, P Tsinganis, A Ulrich, J Urlass, S Valenta, S Vannini, G Variale, V Vaz, P Ventura, A Vescovi, D Vlachoudis, V Vlastou, R Wallner, A Woods, P J Wright, T Žugec, P |
| author_sort | Babiano-Suarez, V |
| collection | CERN |
| description | 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. |
| id | cern-2861329 |
| institution | Organización Europea para la Investigación Nuclear |
| language | eng |
| publishDate | 2022 |
| record_format | invenio |
| spelling | cern-28613292023-06-09T20:08:10Zdoi:10.1051/epjconf/202226011026http://cds.cern.ch/record/2861329engBabiano-Suarez, VBalibrea-Correa, JCaballero-Ontanaya, LDomingo-Pardo, CLadarescu, ILerendegui-Marco, JTain, J LCalviño, FCasanovas, ATarifeño-Saldivia, AGuerrero, CAberle, OAlcayne, VAmaducci, SAndrzejewski, JAudouin, LBacak, MBarbagallo, MBennett, SBerthoumieux, EBillowes, JBosnar, DBrown, ABusso, MCaamaño, MCalviani, MCano-Ott, DCerutti, FChiaveri, EColonna, NCortés, GCortésGiraldo, M ACosentino, LCristallo, SDamone, L ADavies, P JDiakaki, MDietz, MDressler, RDucasse, QDupont, EDurán, IEleme, ZFernández-Domínguez, BFerrari, AFinocchiaro, PFurman, VGöbel, KGarg, RGawlik-Ramięga, AGilardoni, SGonçalves, I FGonzález-Romero, EGunsing, FHarada, HHeinitz, SHeyse, JJenkins, D GJunghans, AKäppeler, FKadi, YKimura, AKnapová, IKokkoris, MKopatch, YKrtička, MKurtulgil, DLederer-Woods, CLeeb, HLonsdale, S JMacina, DManna, AMartínez, TMasi, AMassimi, CMastinu, PMastromarco, MMaugeri, E AMazzone, AMendoza, EMengoni, AMichalopoulou, VMilazzo, P MMingrone, FMoreno-Soto, JMusumarra, ANegret, ANolte, ROgállar, FOprea, APatronis, NPavlik, APerkowski, JPersanti, LPetrone, CPirovano, EPorras, IPraena, JQuesada, J MRamos-Doval, DRauscher, TReifarth, RRochman, DRomanets, YRubbia, CSabaté-Gilarte, MSaxena, ASchillebeeckx, PSchumann, DSekhar, ASmith, A GSosnin, N VSprung, PStamatopoulos, ATagliente, GTassan-Got, LThomas, ThTorres-Sánchez, PTsinganis, AUlrich, JUrlass, SValenta, SVannini, GVariale, VVaz, PVentura, AVescovi, DVlachoudis, VVlastou, RWallner, AWoods, P JWright, TŽugec, PFirst $^{80}$Se(n,$\gamma$) cross section measurement with high resolution in the full stellar energy range 1 eV - 100 keV and its astrophysical implications for the s-processNuclear Physics - ExperimentMost 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.oai:cds.cern.ch:28613292022 |
| spellingShingle | Nuclear Physics - Experiment Babiano-Suarez, V Balibrea-Correa, J Caballero-Ontanaya, L Domingo-Pardo, C Ladarescu, I Lerendegui-Marco, J Tain, J L Calviño, F Casanovas, A Tarifeño-Saldivia, A Guerrero, C Aberle, O Alcayne, V Amaducci, S Andrzejewski, J Audouin, L Bacak, M Barbagallo, M Bennett, S Berthoumieux, E Billowes, J Bosnar, D Brown, A Busso, M Caamaño, M Calviani, M Cano-Ott, D Cerutti, F Chiaveri, E Colonna, N Cortés, G CortésGiraldo, M A Cosentino, L Cristallo, S Damone, L A Davies, P J Diakaki, M Dietz, M Dressler, R Ducasse, Q Dupont, E Durán, I Eleme, Z Fernández-Domínguez, B Ferrari, A Finocchiaro, P Furman, V Göbel, K Garg, R Gawlik-Ramięga, A Gilardoni, S Gonçalves, I F González-Romero, E 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 Krtička, M Kurtulgil, D Lederer-Woods, C Leeb, H Lonsdale, S J Macina, D Manna, A Martínez, T Masi, A Massimi, C Mastinu, P Mastromarco, M Maugeri, E A Mazzone, A Mendoza, E Mengoni, A Michalopoulou, V Milazzo, P M Mingrone, F Moreno-Soto, J Musumarra, A Negret, A Nolte, R Ogállar, F Oprea, A Patronis, N Pavlik, A Perkowski, J Persanti, L Petrone, C Pirovano, E Porras, I Praena, J Quesada, J M Ramos-Doval, D Rauscher, T Reifarth, R Rochman, D Romanets, Y 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 Tassan-Got, L Thomas, Th Torres-Sánchez, P Tsinganis, A Ulrich, J Urlass, S Valenta, S Vannini, G Variale, V Vaz, P Ventura, A Vescovi, D Vlachoudis, V Vlastou, R Wallner, A Woods, P J Wright, T Žugec, P First $^{80}$Se(n,$\gamma$) cross section measurement with high resolution in the full stellar energy range 1 eV - 100 keV and its astrophysical implications for the s-process |
| title | First $^{80}$Se(n,$\gamma$) cross section measurement with high resolution in the full stellar energy range 1 eV - 100 keV and its astrophysical implications for the s-process |
| title_full | First $^{80}$Se(n,$\gamma$) cross section measurement with high resolution in the full stellar energy range 1 eV - 100 keV and its astrophysical implications for the s-process |
| title_fullStr | First $^{80}$Se(n,$\gamma$) cross section measurement with high resolution in the full stellar energy range 1 eV - 100 keV and its astrophysical implications for the s-process |
| title_full_unstemmed | First $^{80}$Se(n,$\gamma$) cross section measurement with high resolution in the full stellar energy range 1 eV - 100 keV and its astrophysical implications for the s-process |
| title_short | First $^{80}$Se(n,$\gamma$) cross section measurement with high resolution in the full stellar energy range 1 eV - 100 keV and its astrophysical implications for the s-process |
| title_sort | first $^{80}$se(n,$\gamma$) cross section measurement with high resolution in the full stellar energy range 1 ev - 100 kev and its astrophysical implications for the s-process |
| topic | Nuclear Physics - Experiment |
| url | https://dx.doi.org/10.1051/epjconf/202226011026 http://cds.cern.ch/record/2861329 |
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first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT musumarraa first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT negreta first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT nolter first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT ogallarf first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT opreaa first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT patronisn first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT pavlika first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT perkowskij first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT persantil first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT petronec first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT pirovanoe first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT porrasi first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT praenaj first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT quesadajm first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT ramosdovald first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT rauschert first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT reifarthr first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT rochmand first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT romanetsy first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT rubbiac first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT sabategilartem first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT saxenaa first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT schillebeeckxp first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT schumannd first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT sekhara first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT smithag first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT sosninnv first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT sprungp first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT stamatopoulosa first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT taglienteg first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT tassangotl first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT thomasth first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT torressanchezp first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT tsinganisa first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT ulrichj first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT urlasss first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT valentas first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT vanninig first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT varialev first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT vazp first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT venturaa first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT vescovid first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT vlachoudisv first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT vlastour first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT wallnera first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT woodspj first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT wrightt first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess AT zugecp first80sengammacrosssectionmeasurementwithhighresolutioninthefullstellarenergyrange1ev100kevanditsastrophysicalimplicationsforthesprocess |