Shedding light on the origin of 204Pb, the heaviest s-process–only isotope in the solar system

Asymptotic giant branch stars are responsible for the production of most of the heavy isotopes beyond Sr observed in the solar system. Among them, isotopes shielded from the ¿-process contribution by their stable isobars are defined as ¿-only nuclei. For a long time the abundance of 204Pb, the heavi...

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Authors: Casanovas Hoste, Adrià|||0000-0002-7138-0894, Domingo Pardo, César, Lerendegui Marco, J., Guerrero, C., Tarifeño Saldivia, Ariel, Krticka, Milan, Pignatari, Marco, Calviño Tavares, Francisco|||0000-0002-7198-4639, Schumann, D., Heinitz, S., Dressler, Rugard, Köster, U., Aberle, Oliver, Andrzejewski, Józef, Audouin, Ludmila, Bécares, Vicente, Bacak, Michael, Balibrea Correa, Javier, Cortés Rossell, Guillem Pere|||0000-0002-3648-5826
Format: article
Publication Date:2024
Country:España
Institution:Universitat Politècnica de Catalunya (UPC)
Repository:UPCommons. Portal del coneixement obert de la UPC
Language:English
OAI Identifier:oai:upcommons.upc.edu:2117/416432
Online Access:https://hdl.handle.net/2117/416432
https://dx.doi.org/10.1103/PhysRevLett.133.052702
Access Level:Open access
Keyword:Isotopes
Neutrons--Capture
Nuclear reactions
Isòtops
Neutrons--Captura
Reaccions nuclears
Àrees temàtiques de la UPC::Física
Àrees temàtiques de la UPC::Energies::Energia nuclear
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oai_identifier_str oai:upcommons.upc.edu:2117/416432
network_acronym_str ES
network_name_str España
repository_id_str
dc.title.none.fl_str_mv Shedding light on the origin of 204Pb, the heaviest s-process–only isotope in the solar system
title Shedding light on the origin of 204Pb, the heaviest s-process–only isotope in the solar system
spellingShingle Shedding light on the origin of 204Pb, the heaviest s-process–only isotope in the solar system
Casanovas Hoste, Adrià|||0000-0002-7138-0894
Isotopes
Neutrons--Capture
Nuclear reactions
Isòtops
Neutrons--Captura
Reaccions nuclears
Àrees temàtiques de la UPC::Física
Àrees temàtiques de la UPC::Energies::Energia nuclear
title_short Shedding light on the origin of 204Pb, the heaviest s-process–only isotope in the solar system
title_full Shedding light on the origin of 204Pb, the heaviest s-process–only isotope in the solar system
title_fullStr Shedding light on the origin of 204Pb, the heaviest s-process–only isotope in the solar system
title_full_unstemmed Shedding light on the origin of 204Pb, the heaviest s-process–only isotope in the solar system
title_sort Shedding light on the origin of 204Pb, the heaviest s-process–only isotope in the solar system
dc.creator.none.fl_str_mv Casanovas Hoste, Adrià|||0000-0002-7138-0894
Domingo Pardo, César
Lerendegui Marco, J.
Guerrero, C.
Tarifeño Saldivia, Ariel
Krticka, Milan
Pignatari, Marco
Calviño Tavares, Francisco|||0000-0002-7198-4639
Schumann, D.
Heinitz, S.
Dressler, Rugard
Köster, U.
Aberle, Oliver
Andrzejewski, Józef
Audouin, Ludmila
Bécares, Vicente
Bacak, Michael
Balibrea Correa, Javier
Cortés Rossell, Guillem Pere|||0000-0002-3648-5826
author Casanovas Hoste, Adrià|||0000-0002-7138-0894
author_facet Casanovas Hoste, Adrià|||0000-0002-7138-0894
Domingo Pardo, César
Lerendegui Marco, J.
Guerrero, C.
Tarifeño Saldivia, Ariel
Krticka, Milan
Pignatari, Marco
Calviño Tavares, Francisco|||0000-0002-7198-4639
Schumann, D.
Heinitz, S.
Dressler, Rugard
Köster, U.
Aberle, Oliver
Andrzejewski, Józef
Audouin, Ludmila
Bécares, Vicente
Bacak, Michael
Balibrea Correa, Javier
Cortés Rossell, Guillem Pere|||0000-0002-3648-5826
author_role author
author2 Domingo Pardo, César
Lerendegui Marco, J.
Guerrero, C.
Tarifeño Saldivia, Ariel
Krticka, Milan
Pignatari, Marco
Calviño Tavares, Francisco|||0000-0002-7198-4639
Schumann, D.
Heinitz, S.
Dressler, Rugard
Köster, U.
Aberle, Oliver
Andrzejewski, Józef
Audouin, Ludmila
Bécares, Vicente
Bacak, Michael
Balibrea Correa, Javier
Cortés Rossell, Guillem Pere|||0000-0002-3648-5826
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Isotopes
Neutrons--Capture
Nuclear reactions
Isòtops
Neutrons--Captura
Reaccions nuclears
Àrees temàtiques de la UPC::Física
Àrees temàtiques de la UPC::Energies::Energia nuclear
topic Isotopes
Neutrons--Capture
Nuclear reactions
Isòtops
Neutrons--Captura
Reaccions nuclears
Àrees temàtiques de la UPC::Física
Àrees temàtiques de la UPC::Energies::Energia nuclear
description Asymptotic giant branch stars are responsible for the production of most of the heavy isotopes beyond Sr observed in the solar system. Among them, isotopes shielded from the ¿-process contribution by their stable isobars are defined as ¿-only nuclei. For a long time the abundance of 204Pb, the heaviest ¿-only isotope, has been a topic of debate because state-of-the-art stellar models appeared to systematically underestimate its solar abundance. Besides the impact of uncertainties from stellar models and galactic chemical evolution simulations, this discrepancy was further obscured by rather divergent theoretical estimates for the neutron capture cross section of its radioactive precursor in the neutron-capture flow, 204Tl (¿1/2=3.78¿¿yr), and by the lack of experimental data on this reaction. We present the first ever neutron capture measurement on 204Tl, conducted at the CERN neutron time-of-flight facility n_TOF, employing a sample of only 9 mg of 204Tl produced at the Institute Laue Langevin high flux reactor. By complementing our new results with semiempirical calculations we obtained, at the ¿-process temperatures of ¿¿¿˜8¿¿keV and ¿¿¿˜30¿¿keV, Maxwellian-averaged cross sections (MACS) of 580(168) mb and 260(90) mb, respectively. These figures are about 3% lower and 20% higher than the corresponding values widely used in astrophysical calculations, which were based only on theoretical calculations. By using the new 204Tl MACS, the uncertainty arising from the 204Tl¿(n,¿) cross section on the ¿-process abundance of 204Pb has been reduced from ~30% down to +8%/-6%, and the ¿-process calculations are in agreement with the latest solar system abundance of 204Pb reported by K. Lodders in 2021.
publishDate 2024
dc.date.none.fl_str_mv 2024
2024-07-31
2024
2024-10-23
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
VoR
http://purl.org/coar/version/c_970fb48d4fbd8a85
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv https://hdl.handle.net/2117/416432
https://dx.doi.org/10.1103/PhysRevLett.133.052702
url https://hdl.handle.net/2117/416432
https://dx.doi.org/10.1103/PhysRevLett.133.052702
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.relation.none.fl_str_mv Ministerio de Economía y Competitividad http://doi.org/10.13039/501100003329 FPA2014-52823-C2-1-P ESTUDIOS DE DESINTEGRACIONES BETA Y DE REACCIONES PARA LA ESTRUCTURA NUCLEAR, ASTROFISICA Y APLICACIONES
Ministerio de Economía y Competitividad http://doi.org/10.13039/501100003329 FPA2014-52823-C2-2-P ESTUDIOS DE DESINTEGRACIONES BETA Y DE REACCIONES PARA LA ESTRUCTURA NUCLEAR, ASTROFISICA Y APLICACIONES
Agencia Estatal de Investigación http://doi.org/10.13039/501100011033 Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016 FPA2017-83946-C2-1-P EXPERIMENTOS DE ESTRUCTURA NUCLEAR Y ASTROFISICA CON HACES RADIOACTIVOS Y NEUTRONES Y APLICACIONES
Agencia Estatal de Investigación http://doi.org/10.13039/501100011033 Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016 FPA2017-83946-C2-2-P EXPERIMENTOS DE ESTRUCTURA NUCLEAR Y ASTROFISICA CON HACES RADIOACTIVOS Y NEUTRONES Y APLICACIONES
Agencia Estatal de Investigación http://doi.org/10.13039/501100011033 Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020 PID2019-104714GB-C21 ESTRUCTURA NUCLEAR, ASTROFISICA Y APLICACIONES - IFIC
Agencia Estatal de Investigación http://doi.org/10.13039/501100011033 Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023 PID2022-138297NB-C21 ESTRUCTURA NUCLEAR, ASTROFISICA Y TRANSFERENCIA DE CONOCIMIENTO IFIC
European Commission http://dx.doi.org/10.13039/100011102 Seventh Framework Programme 334315 NeutAndalus: boosting interdisciplinary neutron science in Spain and Europe
European Commission http://dx.doi.org/10.13039/100011102 Seventh Framework Programme 605203 solving CHAllenges in Nuclear DAta
European Commission http://doi.org/10.13039/100010661 Horizon 2020 Framework Programme 681740 High-sensitivitY Measurements of key stellar Nucleo-Synthesis reactions
European Commission http://doi.org/10.13039/100010661 Horizon 2020 Framework Programme 724560 Radioactivities from Stars to Solar Systems
European Commission http://doi.org/10.13039/100010661 Horizon 2020 Framework Programme 101008324 Chemical Elements as Tracers of the Evolution of the Cosmos
European Commission http://doi.org/10.13039/100010661 Horizon 2020 Framework Programme 677497 Direct measurements of key nuclear Reactions for the creation of Elements in Stars
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
Attribution 4.0 International
http://creativecommons.org/licenses/by/4.0/
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
Attribution 4.0 International
http://creativecommons.org/licenses/by/4.0/
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv American Institute of Physics (AIP)
publisher.none.fl_str_mv American Institute of Physics (AIP)
dc.source.none.fl_str_mv reponame:UPCommons. Portal del coneixement obert de la UPC
instname:Universitat Politècnica de Catalunya (UPC)
instname_str Universitat Politècnica de Catalunya (UPC)
reponame_str UPCommons. Portal del coneixement obert de la UPC
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spelling Shedding light on the origin of 204Pb, the heaviest s-process–only isotope in the solar systemCasanovas Hoste, Adrià|||0000-0002-7138-0894Domingo Pardo, CésarLerendegui Marco, J.Guerrero, C.Tarifeño Saldivia, ArielKrticka, MilanPignatari, MarcoCalviño Tavares, Francisco|||0000-0002-7198-4639Schumann, D.Heinitz, S.Dressler, RugardKöster, U.Aberle, OliverAndrzejewski, JózefAudouin, LudmilaBécares, VicenteBacak, MichaelBalibrea Correa, JavierCortés Rossell, Guillem Pere|||0000-0002-3648-5826IsotopesNeutrons--CaptureNuclear reactionsIsòtopsNeutrons--CapturaReaccions nuclearsÀrees temàtiques de la UPC::FísicaÀrees temàtiques de la UPC::Energies::Energia nuclearAsymptotic giant branch stars are responsible for the production of most of the heavy isotopes beyond Sr observed in the solar system. Among them, isotopes shielded from the ¿-process contribution by their stable isobars are defined as ¿-only nuclei. For a long time the abundance of 204Pb, the heaviest ¿-only isotope, has been a topic of debate because state-of-the-art stellar models appeared to systematically underestimate its solar abundance. Besides the impact of uncertainties from stellar models and galactic chemical evolution simulations, this discrepancy was further obscured by rather divergent theoretical estimates for the neutron capture cross section of its radioactive precursor in the neutron-capture flow, 204Tl (¿1/2=3.78¿¿yr), and by the lack of experimental data on this reaction. We present the first ever neutron capture measurement on 204Tl, conducted at the CERN neutron time-of-flight facility n_TOF, employing a sample of only 9 mg of 204Tl produced at the Institute Laue Langevin high flux reactor. By complementing our new results with semiempirical calculations we obtained, at the ¿-process temperatures of ¿¿¿˜8¿¿keV and ¿¿¿˜30¿¿keV, Maxwellian-averaged cross sections (MACS) of 580(168) mb and 260(90) mb, respectively. These figures are about 3% lower and 20% higher than the corresponding values widely used in astrophysical calculations, which were based only on theoretical calculations. By using the new 204Tl MACS, the uncertainty arising from the 204Tl¿(n,¿) cross section on the ¿-process abundance of 204Pb has been reduced from ~30% down to +8%/-6%, and the ¿-process calculations are in agreement with the latest solar system abundance of 204Pb reported by K. Lodders in 2021.We acknowledge the suggestions of three referees, which helped to improve the present article in several relevant aspects. We would like to acknowledge financial support from the Argos Scholarship of the Universtitat Politècnica de Catalunya (UPC) and the Consejo de Seguridad Nuclear (CSN), the Spanish Government Ministries MINECO (projects FPA2014- 52823-C2-1/2-P and FPA2017-83946-C2-1/2-P) and MCIU (projects PID2019–104714 GB-C21 and PID2022-138297NB-C21), the EC FP7 projects NeutAndalus (Grant No. 334315) and CHANDA (Grant No. 605203), and the n_TOF Collaboration and the Institut de Tècniques Energètiques (INTE) of the UPC. A. C. H. also recognizes the support from a Margarita Salas grant by the UPC (Agreement CG/2021/03/23) funded by the Ministerio de Universidades (Order UNI/551/2021) and by the European Union NextGenerationEU/PRTR. A. C. H. and C. D. P. acknowledge support from ERC Consolidator Grant HYMNS, Grant Agreement No. 681740. M. P. acknowledges significant support to NuGrid from STFC (through the University of Hull’s Consolidated Grant No. ST/R000840/1), from the ERC Consolidator Grant FIG. 3. Isotopic abundance ratios Nð204PbÞ=Nð150SmÞ in the star envelope at the end of the AGB phase, obtained using the MACS from Fig. 2 for the stellar models described in the text. All values are normalized to the solar system (ss) ratio [10], which is highlighted by the thick green bar with the green shaded band depicting its uncertainty. Solid error bars reflect only the uncertainty contribution from the cross section, while dashed error bars include also the uncertainty on the thermal dependency of the β− decay of 204Tl [31]. PHYSICAL REVIEW LETTERS 133, 052702 (2024) 052702-6 (Hungary) funding scheme (Project RADIOSTAR, G. A. n. 724560), from the ChETEC COST Action (CA16117), supported by the European Cooperation in Science and Technology, from the IReNA network supported by NSF AccelNet, from the National Science Foundation (NSF, USA) under Grant No. PHY-1430152 (JINA Center for the Evolution of the Elements), from the NKFI via K-project 138031 and the Lendület Program LP2023-10 of the Hungarian Academy of Sciences and from the European Union’s Horizon 2020 research and innovation programme (ChETEC-INFRA—Project No. 101008324). M. P. also acknowledges the access to VIPER, the University of Hull High Performance Computing Facility. C. L. W. acknowl- edges support from the Science and Technology Facilities Council UK (ST/M006085/1), and the European Research Council ERC-2015-STG No. 677497. The support of all funding agencies of the n_TOF participating institutes is acknowledged.Article signat per 134 autors/es: A. Casanovas-Hoste, C. Domingo-Pardo, J. Lerendegui-Marco, C. Guerrero, A. Tarifeño-Saldivia, M. Krtička, M. Pignatari, F. Calviño, D. Schumann, S. Heinitz, R. Dressler, U. Köster, O. Aberle, J. Andrzejewski, L. Audouin, V. Bécares, M. Bacak, J. Balibrea-Correa, M. Barbagallo, S. Barros, F. Bečvář, C. Beinrucker, E. Berthoumieux, J. Billowes, D. Bosnar, M. Brugger, M. Caamaño, M. Calviani, D. Cano-Ott, R. Cardella, D. M. Castelluccio, F. Cerutti, Y. H. Chen, E. Chiaveri, N. Colonna, G. Cortés, M. A. Cortés-Giraldo, L. Cosentino, L. A. Damone, M. Diakaki, E. Dupont, I. Durán, B. Fernández-Domínguez, A. Ferrari, P. Ferreira, P. Finocchiaro, V. Furman, K. Göbel, A. R. García, A. Gawlik-Ramięga, T. Glodariu, I. F. Gonçalves, E. González-Romero, A. Goverdovski, E. Griesmayer, F. Gunsing, H. Harada, T. Heftrich, J. Heyse, D. G. Jenkins, E. Jericha, F. Käppeler, Y. Kadi, T. Katabuchi, P. Kavrigin, V. Ketlerov, V. Khryachkov, A. Kimura, N. Kivel, M. Kokkoris, E. Leal-Cidoncha, C. Lederer-Woods, H. Leeb, S. Lo Meo, S. J. Lonsdale, R. Losito, D. Macina, J. Marganiec, T. Martínez, C. Massimi, P. Mastinu, M. Mastromarco, F. Matteucci, E. A. Maugeri, E. Mendoza, A. Mengoni, P. M. Milazzo, F. Mingrone, M. Mirea, S. Montesano, A. Musumarra, R. Nolte, A. Oprea, N. Patronis, A. Pavlik, J. Perkowski, I. Porras, J. Praena, J. M. Quesada, K. Rajeev, T. Rauscher, R. Reifarth, A. Riego-Perez, Y. Romanets, P. C. Rout, C. Rubbia, J. A. Ryan, M. Sabaté-Gilarte, A. Saxena, P. Schillebeeckx, S. Schmidt, P. Sedyshev, A. G. Smith, A. Stamatopoulos, G. Tagliente, J. L. Tain, L. Tassan-Got, A. Tsinganis, S. Valenta, G. Vannini, V. Variale, P. Vaz, A. Ventura, V. Vlachoudis, R. Vlastou, A. Wallner, S. Warren, M. Weigand, C. Weiss, C. Wolf, P. J. Woods, T. Wright, P. Žugec.American Institute of Physics (AIP)20242024-07-3120242024-10-23journal articlehttp://purl.org/coar/resource_type/c_6501VoRhttp://purl.org/coar/version/c_970fb48d4fbd8a85info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/2117/416432https://dx.doi.org/10.1103/PhysRevLett.133.052702reponame:UPCommons. Portal del coneixement obert de la UPCinstname:Universitat Politècnica de Catalunya (UPC)InglésengMinisterio de Economía y Competitividad http://doi.org/10.13039/501100003329 FPA2014-52823-C2-1-P ESTUDIOS DE DESINTEGRACIONES BETA Y DE REACCIONES PARA LA ESTRUCTURA NUCLEAR, ASTROFISICA Y APLICACIONESMinisterio de Economía y Competitividad http://doi.org/10.13039/501100003329 FPA2014-52823-C2-2-P ESTUDIOS DE DESINTEGRACIONES BETA Y DE REACCIONES PARA LA ESTRUCTURA NUCLEAR, ASTROFISICA Y APLICACIONESAgencia Estatal de Investigación http://doi.org/10.13039/501100011033 Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016 FPA2017-83946-C2-1-P EXPERIMENTOS DE ESTRUCTURA NUCLEAR Y ASTROFISICA CON HACES RADIOACTIVOS Y NEUTRONES Y APLICACIONESAgencia Estatal de Investigación http://doi.org/10.13039/501100011033 Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016 FPA2017-83946-C2-2-P EXPERIMENTOS DE ESTRUCTURA NUCLEAR Y ASTROFISICA CON HACES RADIOACTIVOS Y NEUTRONES Y APLICACIONESAgencia Estatal de Investigación http://doi.org/10.13039/501100011033 Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020 PID2019-104714GB-C21 ESTRUCTURA NUCLEAR, ASTROFISICA Y APLICACIONES - IFICAgencia Estatal de Investigación http://doi.org/10.13039/501100011033 Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023 PID2022-138297NB-C21 ESTRUCTURA NUCLEAR, ASTROFISICA Y TRANSFERENCIA DE CONOCIMIENTO IFICEuropean Commission http://dx.doi.org/10.13039/100011102 Seventh Framework Programme 334315 NeutAndalus: boosting interdisciplinary neutron science in Spain and EuropeEuropean Commission http://dx.doi.org/10.13039/100011102 Seventh Framework Programme 605203 solving CHAllenges in Nuclear DAtaEuropean Commission http://doi.org/10.13039/100010661 Horizon 2020 Framework Programme 681740 High-sensitivitY Measurements of key stellar Nucleo-Synthesis reactionsEuropean Commission http://doi.org/10.13039/100010661 Horizon 2020 Framework Programme 724560 Radioactivities from Stars to Solar SystemsEuropean Commission http://doi.org/10.13039/100010661 Horizon 2020 Framework Programme 101008324 Chemical Elements as Tracers of the Evolution of the CosmosEuropean Commission http://doi.org/10.13039/100010661 Horizon 2020 Framework Programme 677497 Direct measurements of key nuclear Reactions for the creation of Elements in Starsopen accesshttp://purl.org/coar/access_right/c_abf2Attribution 4.0 Internationalhttp://creativecommons.org/licenses/by/4.0/info:eu-repo/semantics/openAccessoai:upcommons.upc.edu:2117/4164322026-05-27T15:37:01Z
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