Nucleosynthetic yields of intermediate-mass primordial to extremely metal-poor stars

Stellar models and nucleosynthetic yields of primordial to extremely metal-poor (EMP) stars are crucial to interpret the surface abundances of the most metal-poor stars observed and, ultimately, to better understand the earliest stellar populations. In addition, they are key ingredients of Galactic...

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Authors: Gil Pons, Pilar|||0000-0001-5410-3564, Doherty, Carolyn, Campbell, Simon W, Gutiérrez Cabello, Jordi|||0000-0003-1978-3642
Format: article
Publication Date:2022
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:2117/386103
Online Access:https://hdl.handle.net/2117/386103
https://dx.doi.org/10.1051/0004-6361/202244062
Access Level:Open access
Keyword:Stars--Evolution
Asymptotic giant branch stars
Nuclear reactions
nucleosynthesis
abundances
Stars -- evolution
Stars -- population II
Stars -- AGB and post-AGB
ISM -- abundances
Estels--Evolució
Àrees temàtiques de la UPC::Física::Astronomia i astrofísica
id ES_7d8630bd2e2872302a0c5409d906e438
oai_identifier_str oai:upcommons.upc.edu:2117/386103
network_acronym_str ES
network_name_str España
repository_id_str
dc.title.none.fl_str_mv Nucleosynthetic yields of intermediate-mass primordial to extremely metal-poor stars
title Nucleosynthetic yields of intermediate-mass primordial to extremely metal-poor stars
spellingShingle Nucleosynthetic yields of intermediate-mass primordial to extremely metal-poor stars
Gil Pons, Pilar|||0000-0001-5410-3564
Stars--Evolution
Asymptotic giant branch stars
Nuclear reactions
nucleosynthesis
abundances
Stars -- evolution
Stars -- population II
Stars -- AGB and post-AGB
ISM -- abundances
Estels--Evolució
Àrees temàtiques de la UPC::Física::Astronomia i astrofísica
title_short Nucleosynthetic yields of intermediate-mass primordial to extremely metal-poor stars
title_full Nucleosynthetic yields of intermediate-mass primordial to extremely metal-poor stars
title_fullStr Nucleosynthetic yields of intermediate-mass primordial to extremely metal-poor stars
title_full_unstemmed Nucleosynthetic yields of intermediate-mass primordial to extremely metal-poor stars
title_sort Nucleosynthetic yields of intermediate-mass primordial to extremely metal-poor stars
dc.creator.none.fl_str_mv Gil Pons, Pilar|||0000-0001-5410-3564
Doherty, Carolyn
Campbell, Simon W
Gutiérrez Cabello, Jordi|||0000-0003-1978-3642
author Gil Pons, Pilar|||0000-0001-5410-3564
author_facet Gil Pons, Pilar|||0000-0001-5410-3564
Doherty, Carolyn
Campbell, Simon W
Gutiérrez Cabello, Jordi|||0000-0003-1978-3642
author_role author
author2 Doherty, Carolyn
Campbell, Simon W
Gutiérrez Cabello, Jordi|||0000-0003-1978-3642
author2_role author
author
author
dc.subject.none.fl_str_mv Stars--Evolution
Asymptotic giant branch stars
Nuclear reactions
nucleosynthesis
abundances
Stars -- evolution
Stars -- population II
Stars -- AGB and post-AGB
ISM -- abundances
Estels--Evolució
Àrees temàtiques de la UPC::Física::Astronomia i astrofísica
topic Stars--Evolution
Asymptotic giant branch stars
Nuclear reactions
nucleosynthesis
abundances
Stars -- evolution
Stars -- population II
Stars -- AGB and post-AGB
ISM -- abundances
Estels--Evolució
Àrees temàtiques de la UPC::Física::Astronomia i astrofísica
description Stellar models and nucleosynthetic yields of primordial to extremely metal-poor (EMP) stars are crucial to interpret the surface abundances of the most metal-poor stars observed and, ultimately, to better understand the earliest stellar populations. In addition, they are key ingredients of Galactic chemical evolution models. Aims. We aim to better characterise the evolution and fates, and determine updated nucleosynthetic yields of intermediate-mass stars between primordial and EMP metallicity (Z = 10-10, 10-8, 10-7, 10-6, and 10-5). We also probed uncertainties in the nucleosynthesis of the oldest intermediate-mass stars, namely those related to the treatment of convection and convective boundaries and those related to wind prescriptions during the asymptotic giant branch (AGB) phase. Methods. We analyse the evolution of models from their main sequence, through the thermally pulsing AGB (TP-AGB), to the latest stages of their evolution, using the Monash-Mount Stromlo stellar evolution code MONSTAR. The results were post-processed with the code MONSOON, which allowed for the determination of the nucleosynthetic yields of 77 species up to 62Ni. By comparing them to similar calculations existing in the literature, we inspected the effects of input physics on the nucleosynthesis of EMP models. Results. From the evolutionary point of view, as reported in former works, we identified proton ingestion episodes (PIEs) in our lowest-mass lowest-metallicity models. Models of Z = 10-10 and Z = 10-8 in a narrow initial mass range around 5 M experience the cessation of thermal pulses, and their final fates as type-I1/2 supernovae cannot be discarded. However, the initial mass range of models eventually leading to the formation of type-I1/2 and electron-capture supernovae is considerably reduced compared to former works. All the models of initial mass & 6-7 M experience a corrosive second dredge-up and, analogously to those experiencing PIEs, undergo significant metal enrichment in their envelopes. The associated increase in their opacities allows them to develop a solar-like TP-AGB or TP-super-AGB, ultimately becoming white dwarfs. Except for those undergoing the cessation of thermal pulses, all of our models show the nucleosynthetic signatures of both efficient third dredge-up and hot-bottom burning, with the activation of the NeNa cycle and the MgAlSi chains. This leads to the creation of vast amounts of CNO, with typical [N/Fe] > 4), and the characteristic abundance signature [N/Fe] > [C/Fe] > [O/Fe]. Our nucleosynthetic yields present dramatic differences with respect to recent results existing in the literature for intermediate-mass models of similar metallicities. The reason for these discrepancies lay in the poorly known input physics related to stellar winds and, above all, the treatment of convection and convective boundaries.
publishDate 2022
dc.date.none.fl_str_mv 2022
2022-12-01
2023
2023-04-12
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
CVoR
http://purl.org/coar/version/c_e19f295774971610
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv https://hdl.handle.net/2117/386103
https://dx.doi.org/10.1051/0004-6361/202244062
url https://hdl.handle.net/2117/386103
https://dx.doi.org/10.1051/0004-6361/202244062
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
Attribution-NonCommercial-NoDerivatives 4.0 International
http://creativecommons.org/licenses/by-nc-nd/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-NonCommercial-NoDerivatives 4.0 International
http://creativecommons.org/licenses/by-nc-nd/4.0/
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: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
collection UPCommons. Portal del coneixement obert de la UPC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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spelling Nucleosynthetic yields of intermediate-mass primordial to extremely metal-poor starsGil Pons, Pilar|||0000-0001-5410-3564Doherty, CarolynCampbell, Simon WGutiérrez Cabello, Jordi|||0000-0003-1978-3642Stars--EvolutionAsymptotic giant branch starsNuclear reactionsnucleosynthesisabundancesStars -- evolutionStars -- population IIStars -- AGB and post-AGBISM -- abundancesEstels--EvolucióÀrees temàtiques de la UPC::Física::Astronomia i astrofísicaStellar models and nucleosynthetic yields of primordial to extremely metal-poor (EMP) stars are crucial to interpret the surface abundances of the most metal-poor stars observed and, ultimately, to better understand the earliest stellar populations. In addition, they are key ingredients of Galactic chemical evolution models. Aims. We aim to better characterise the evolution and fates, and determine updated nucleosynthetic yields of intermediate-mass stars between primordial and EMP metallicity (Z = 10-10, 10-8, 10-7, 10-6, and 10-5). We also probed uncertainties in the nucleosynthesis of the oldest intermediate-mass stars, namely those related to the treatment of convection and convective boundaries and those related to wind prescriptions during the asymptotic giant branch (AGB) phase. Methods. We analyse the evolution of models from their main sequence, through the thermally pulsing AGB (TP-AGB), to the latest stages of their evolution, using the Monash-Mount Stromlo stellar evolution code MONSTAR. The results were post-processed with the code MONSOON, which allowed for the determination of the nucleosynthetic yields of 77 species up to 62Ni. By comparing them to similar calculations existing in the literature, we inspected the effects of input physics on the nucleosynthesis of EMP models. Results. From the evolutionary point of view, as reported in former works, we identified proton ingestion episodes (PIEs) in our lowest-mass lowest-metallicity models. Models of Z = 10-10 and Z = 10-8 in a narrow initial mass range around 5 M experience the cessation of thermal pulses, and their final fates as type-I1/2 supernovae cannot be discarded. However, the initial mass range of models eventually leading to the formation of type-I1/2 and electron-capture supernovae is considerably reduced compared to former works. All the models of initial mass & 6-7 M experience a corrosive second dredge-up and, analogously to those experiencing PIEs, undergo significant metal enrichment in their envelopes. The associated increase in their opacities allows them to develop a solar-like TP-AGB or TP-super-AGB, ultimately becoming white dwarfs. Except for those undergoing the cessation of thermal pulses, all of our models show the nucleosynthetic signatures of both efficient third dredge-up and hot-bottom burning, with the activation of the NeNa cycle and the MgAlSi chains. This leads to the creation of vast amounts of CNO, with typical [N/Fe] > 4), and the characteristic abundance signature [N/Fe] > [C/Fe] > [O/Fe]. Our nucleosynthetic yields present dramatic differences with respect to recent results existing in the literature for intermediate-mass models of similar metallicities. The reason for these discrepancies lay in the poorly known input physics related to stellar winds and, above all, the treatment of convection and convective boundaries.We thank the anonymous referee for their useful comments and clarifications. This work was supported by the Spanish project PID 2019-109363GB-100, and by the German Deutsche Forschungsgemeinschaft, DFG project number Ts 17/2–1. S.W.C. acknowledges federal funding from the Australian Research Council through a Future Fellowship (FT160100046) and Discovery Project (DP190102431). This research was supported by use of the Nectar Research Cloud, a collaborative Australian research platform supported by the National Collaborative Research Infrastructure Strategy (NCRIS).We thank the anonymous referee for their useful comments and clarifications. This work was supported by the Spanish project PID 2019-109363GB-100, and by the German Deutsche Forschungsgemeinschaft, DFG project number Ts 17/2–1. S.W.C. acknowledges federal funding from the Australian Research Council through a Future Fellowship (FT160100046) and Discovery Project (DP190102431). This research was supported by use of the Nectar Research Cloud, a collaborative Australian research platform supported by the National Collaborative Research Infrastructure Strategy (NCRIS).Peer ReviewedEDP Sciences20222022-12-0120232023-04-12journal articlehttp://purl.org/coar/resource_type/c_6501CVoRhttp://purl.org/coar/version/c_e19f295774971610info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/2117/386103https://dx.doi.org/10.1051/0004-6361/202244062reponame:UPCommons. Portal del coneixement obert de la UPCinstname:Universitat Politècnica de Catalunya (UPC)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2Attribution-NonCommercial-NoDerivatives 4.0 Internationalhttp://creativecommons.org/licenses/by-nc-nd/4.0/info:eu-repo/semantics/openAccessoai:upcommons.upc.edu:2117/3861032026-05-27T15:37:01Z
score 15,301603

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