The i-processes nucleosynthesis during the formation of He-rich hot-subdwarf stars

[Context] Intermediate neutron-capture processes are thought to occur in stellar environments where protons are ingested into a hot helium-burning convective region. It has been shown that proton ingestion episodes can happen in the formation of hot-subdwarf stars, and that neutron-capture processes...

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Autores: Battich, Tiara, Miller Bertolami, Marcelo M., Weiss, Achim, Dorsch, M., Serenelli, Aldo, Justham, Stephen
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2025
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/398702
Acceso en línea:http://hdl.handle.net/10261/398702
Access Level:acceso abierto
Palabra clave:Nuclear reactions, nucleosynthesis, abundances
Stars: evolution
Stars: low-mass
Subdwarfs
id ES_110a6257a5bcfaf7dca74572572fd8dc
oai_identifier_str oai:digital.csic.es:10261/398702
network_acronym_str ES
network_name_str España
repository_id_str
dc.title.none.fl_str_mv The i-processes nucleosynthesis during the formation of He-rich hot-subdwarf stars
title The i-processes nucleosynthesis during the formation of He-rich hot-subdwarf stars
spellingShingle The i-processes nucleosynthesis during the formation of He-rich hot-subdwarf stars
Battich, Tiara
Nuclear reactions, nucleosynthesis, abundances
Stars: evolution
Stars: low-mass
Subdwarfs
title_short The i-processes nucleosynthesis during the formation of He-rich hot-subdwarf stars
title_full The i-processes nucleosynthesis during the formation of He-rich hot-subdwarf stars
title_fullStr The i-processes nucleosynthesis during the formation of He-rich hot-subdwarf stars
title_full_unstemmed The i-processes nucleosynthesis during the formation of He-rich hot-subdwarf stars
title_sort The i-processes nucleosynthesis during the formation of He-rich hot-subdwarf stars
dc.creator.none.fl_str_mv Battich, Tiara
Miller Bertolami, Marcelo M.
Weiss, Achim
Dorsch, M.
Serenelli, Aldo
Justham, Stephen
author Battich, Tiara
author_facet Battich, Tiara
Miller Bertolami, Marcelo M.
Weiss, Achim
Dorsch, M.
Serenelli, Aldo
Justham, Stephen
author_role author
author2 Miller Bertolami, Marcelo M.
Weiss, Achim
Dorsch, M.
Serenelli, Aldo
Justham, Stephen
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv German Research Foundation
Consejo Nacional de Investigaciones Científicas y Técnicas (Argentina)
German Academic Exchange Service
German Centre for Air and Space Travel
Ministerio de Ciencia, Innovación y Universidades (España)
Generalitat de Catalunya
Agencia Estatal de Investigación (España)
Ministerio de Ciencia e Innovación (España)
Miller Bertolami, Marcelo M. [0000-0001-8031-1957]
Serenelli, Aldo [0000-0001-6359-2769]
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Nuclear reactions, nucleosynthesis, abundances
Stars: evolution
Stars: low-mass
Subdwarfs
topic Nuclear reactions, nucleosynthesis, abundances
Stars: evolution
Stars: low-mass
Subdwarfs
description [Context] Intermediate neutron-capture processes are thought to occur in stellar environments where protons are ingested into a hot helium-burning convective region. It has been shown that proton ingestion episodes can happen in the formation of hot-subdwarf stars, and that neutron-capture processes are possible in those cases. Moreover, some helium-rich hot subdwarfs display extraordinarily high abundances of heavy elements such as Zr, Yr, and Pb on their surfaces. These elements can be produced by both slow and intermediate neutron-capture processes.
publishDate 2025
dc.date.none.fl_str_mv 2025
2025
2025
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_dcae04bc
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/398702
url http://hdl.handle.net/10261/398702
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
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info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/PID2023-149918NB-I00
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/CEX2020-001058-M
https://doi.org/10.1051/0004-6361/202453572
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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spelling The i-processes nucleosynthesis during the formation of He-rich hot-subdwarf starsBattich, TiaraMiller Bertolami, Marcelo M.Weiss, AchimDorsch, M.Serenelli, AldoJustham, StephenNuclear reactions, nucleosynthesis, abundancesStars: evolutionStars: low-massSubdwarfs[Context] Intermediate neutron-capture processes are thought to occur in stellar environments where protons are ingested into a hot helium-burning convective region. It has been shown that proton ingestion episodes can happen in the formation of hot-subdwarf stars, and that neutron-capture processes are possible in those cases. Moreover, some helium-rich hot subdwarfs display extraordinarily high abundances of heavy elements such as Zr, Yr, and Pb on their surfaces. These elements can be produced by both slow and intermediate neutron-capture processes.[Aims] We explore under which conditions neutron-capture processes can occur in late helium core flashes, that is, those occurring in the cores of stripped red-giant stars. We explore the dependence of such processes on the metallicity of the star, and how much the star is stripped before the He flash takes place.[Methods] We computed evolutionary models through the helium core flash and the subsequent hydrogen ingestion episode in stripped red-giant stars. Stellar structure models were then used in post-processing to compute the detailed evolution of neutron-capture elements.[Results] We find that for metallicities of 10−3 and below, neutron densities can be as high as 1015 cm−3 and intermediate neutron-capture processes occur in some of our models. The results depend very strongly on the H-envelope mass that survives after the stripping, which alters the nucleosynthesis during the flashes, and therefore the behavior of the convective motions. Interestingly, we find that computed abundances in some of our models closely match the element abundances up to tin observed for EC 22536-5304, the only well-studied star for which the hot-flasher scenario assumed in our models is the most likely evolutionary path.[Conclusions] Intermediate neutron-capture processes can occur in the He-core flash experienced by the cores of some stripped red giants, and this might be connected to the abundances of heavy elements observed in some helium-rich hot-subdwarf stars. The agreement between the observed abundances in EC 22536-5304 and those of our models offers support to our nucleosynthesis calculations. Moreover, if confirmed, the idea that heavy element abundances retain signatures of the different evolutionary channels opens the possibility that heavy element abundances in iHe-sdOB stars can be used to infer their evolutionary origin.We thank the referee for the constructive report, which helped to improve this work. T.B. thanks S.E. de Mink for useful discussions regarding the presentation of this work. Part of this work was supported by the German Deutsche Forschungsgemeinschaft, DFG project number Ts 17/2–1.This research was supported by the Munich Institute for Astro-, Particle and BioPhysics (MIAPbP) which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy – EXC-2094 – 390783311. Part of this work was supported by the CONICET-DAAD 2022 bilateral cooperation grant number 80726. M3B is partially funded by CONICET and Agencia I+D+i through grants PIP-2971 and PICT 2020-03316. Matti Dorsch is supported by the Deutsches Zentrum für Luft- und Raumfahrt (DLR) through grant 50-OR-2304. A.S. acknowledges support by the Spanish Ministry of Science, Innovation and Universities through the grant PID2023-149918NB-I00 and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M, and by Generalitat de Catalunya through grant 2021-SGR-1526.With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (CEX2020-001058-M)Peer reviewedEDP SciencesGerman Research FoundationConsejo Nacional de Investigaciones Científicas y Técnicas (Argentina)German Academic Exchange ServiceGerman Centre for Air and Space TravelMinisterio de Ciencia, Innovación y Universidades (España)Generalitat de CatalunyaAgencia Estatal de Investigación (España)Ministerio de Ciencia e Innovación (España)Miller Bertolami, Marcelo M. [0000-0001-8031-1957]Serenelli, Aldo [0000-0001-6359-2769]Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202520252025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_dcae04bcPublisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/398702reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/PID2023-149918NB-I00info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/CEX2020-001058-Mhttps://doi.org/10.1051/0004-6361/202453572Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3987022026-05-22T06:33:51Z
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