Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMa

Autores
Sánchez Arias, Julieta Paz; Németh, Péter; Saldanha da Gama de Almeida, Elisson; Ruiz Diaz, Matias Agustin; Kraus, Michaela; Haucke, Maximiliano
Año de publicación
2023
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We aim to combine asteroseismology, spectroscopy, and evolutionary models to establisha comprehensive picture of the evolution of Galactic blue supergiant stars (BSG). To start such aninvestigation, we selected three BSG candidates for our analysis: HD 42087 (PU Gem), HD 52089(e CMa), and HD 58350 (η CMa). These stars show pulsations and were suspected to be in anevolutionary stage either preceding or succeding the red supergiant (RSG) stage. For our analysis,we utilized the 2-min cadence TESS data to study the photometric variability, and we obtained newspectroscopic observations at the CASLEO observatory. We used non-LTE radiative transfer modelscalculated with CMFGEN to derive their stellar and wind parameters. For the fitting procedure,we included CMFGEN models in the iterative spectral analysis pipeline XTGRID to determine theirCNO abundances. The spectral modeling was limited to changing only the effective temperature,surface gravity, CNO abundances, and mass-loss rates. Finally, we compared the derived metalabundances with prediction from Geneva stellar evolution models. The frequency spectra of all threestars show stochastic oscillations and indications of one nonradial strange mode, fr = 0.09321 d−1inHD 42087 and a rotational splitting centred in f2 = 0.36366 d−1in HD 52089. We conclude that therather short sectoral observing windows of TESS prevent establishing a reliable mode identificationof low frequencies connected to mass-loss variabilities. The spectral analysis confirmed gradualchanges in the mass-loss rates, and the derived CNO abundances comply with the values reportedin the literature. We were able to achieve a quantitative match with stellar evolution models for thestellar masses and luminosities. However, the spectroscopic surface abundances turned out to beinconsistent with the theoretical predictions. The stars show N enrichment, typical for CNO cycleprocessed material, but the abundance ratios did not reflect the associated levels of C and O depletion.We found HD 42087 to be the most consistent with a pre-RSG evolutionary stage, HD 58350 is mostlikely in a post-RSG evolution and HD 52089 shows stellar parameters compatible with a star atthe TAMS.
Fil: Sánchez Arias, Julieta Paz. Czech Academy of Sciences; República Checa. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Németh, Péter. Czech Academy of Sciences; República Checa
Fil: Saldanha da Gama de Almeida, Elisson. Universidad de Valparaíso; Chile
Fil: Ruiz Diaz, Matias Agustin. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Kraus, Michaela. Czech Academy of Sciences; República Checa
Fil: Haucke, Maximiliano. Universidad Nacional de La Plata; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Materia
MASSIVE STARS
SUPERGIANTS
OUTFLOWS
WINDS
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/236319

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repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMaSánchez Arias, Julieta PazNémeth, PéterSaldanha da Gama de Almeida, ElissonRuiz Diaz, Matias AgustinKraus, MichaelaHaucke, MaximilianoMASSIVE STARSSUPERGIANTSOUTFLOWSWINDShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We aim to combine asteroseismology, spectroscopy, and evolutionary models to establisha comprehensive picture of the evolution of Galactic blue supergiant stars (BSG). To start such aninvestigation, we selected three BSG candidates for our analysis: HD 42087 (PU Gem), HD 52089(e CMa), and HD 58350 (η CMa). These stars show pulsations and were suspected to be in anevolutionary stage either preceding or succeding the red supergiant (RSG) stage. For our analysis,we utilized the 2-min cadence TESS data to study the photometric variability, and we obtained newspectroscopic observations at the CASLEO observatory. We used non-LTE radiative transfer modelscalculated with CMFGEN to derive their stellar and wind parameters. For the fitting procedure,we included CMFGEN models in the iterative spectral analysis pipeline XTGRID to determine theirCNO abundances. The spectral modeling was limited to changing only the effective temperature,surface gravity, CNO abundances, and mass-loss rates. Finally, we compared the derived metalabundances with prediction from Geneva stellar evolution models. The frequency spectra of all threestars show stochastic oscillations and indications of one nonradial strange mode, fr = 0.09321 d−1inHD 42087 and a rotational splitting centred in f2 = 0.36366 d−1in HD 52089. We conclude that therather short sectoral observing windows of TESS prevent establishing a reliable mode identificationof low frequencies connected to mass-loss variabilities. The spectral analysis confirmed gradualchanges in the mass-loss rates, and the derived CNO abundances comply with the values reportedin the literature. We were able to achieve a quantitative match with stellar evolution models for thestellar masses and luminosities. However, the spectroscopic surface abundances turned out to beinconsistent with the theoretical predictions. The stars show N enrichment, typical for CNO cycleprocessed material, but the abundance ratios did not reflect the associated levels of C and O depletion.We found HD 42087 to be the most consistent with a pre-RSG evolutionary stage, HD 58350 is mostlikely in a post-RSG evolution and HD 52089 shows stellar parameters compatible with a star atthe TAMS.Fil: Sánchez Arias, Julieta Paz. Czech Academy of Sciences; República Checa. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Németh, Péter. Czech Academy of Sciences; República ChecaFil: Saldanha da Gama de Almeida, Elisson. Universidad de Valparaíso; ChileFil: Ruiz Diaz, Matias Agustin. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Kraus, Michaela. Czech Academy of Sciences; República ChecaFil: Haucke, Maximiliano. Universidad Nacional de La Plata; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaMDPI2023-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/236319Sánchez Arias, Julieta Paz; Németh, Péter; Saldanha da Gama de Almeida, Elisson; Ruiz Diaz, Matias Agustin; Kraus, Michaela; et al.; Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMa; MDPI; Galaxies; 11; 5; 8-2023; 93-1222075-4434CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.mdpi.com/2075-4434/11/5/93info:eu-repo/semantics/altIdentifier/doi/10.3390/galaxies11050093info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:23:22Zoai:ri.conicet.gov.ar:11336/236319instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-22 11:23:23.138CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMa
title Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMa
spellingShingle Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMa
Sánchez Arias, Julieta Paz
MASSIVE STARS
SUPERGIANTS
OUTFLOWS
WINDS
title_short Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMa
title_full Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMa
title_fullStr Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMa
title_full_unstemmed Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMa
title_sort Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMa
dc.creator.none.fl_str_mv Sánchez Arias, Julieta Paz
Németh, Péter
Saldanha da Gama de Almeida, Elisson
Ruiz Diaz, Matias Agustin
Kraus, Michaela
Haucke, Maximiliano
author Sánchez Arias, Julieta Paz
author_facet Sánchez Arias, Julieta Paz
Németh, Péter
Saldanha da Gama de Almeida, Elisson
Ruiz Diaz, Matias Agustin
Kraus, Michaela
Haucke, Maximiliano
author_role author
author2 Németh, Péter
Saldanha da Gama de Almeida, Elisson
Ruiz Diaz, Matias Agustin
Kraus, Michaela
Haucke, Maximiliano
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv MASSIVE STARS
SUPERGIANTS
OUTFLOWS
WINDS
topic MASSIVE STARS
SUPERGIANTS
OUTFLOWS
WINDS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We aim to combine asteroseismology, spectroscopy, and evolutionary models to establisha comprehensive picture of the evolution of Galactic blue supergiant stars (BSG). To start such aninvestigation, we selected three BSG candidates for our analysis: HD 42087 (PU Gem), HD 52089(e CMa), and HD 58350 (η CMa). These stars show pulsations and were suspected to be in anevolutionary stage either preceding or succeding the red supergiant (RSG) stage. For our analysis,we utilized the 2-min cadence TESS data to study the photometric variability, and we obtained newspectroscopic observations at the CASLEO observatory. We used non-LTE radiative transfer modelscalculated with CMFGEN to derive their stellar and wind parameters. For the fitting procedure,we included CMFGEN models in the iterative spectral analysis pipeline XTGRID to determine theirCNO abundances. The spectral modeling was limited to changing only the effective temperature,surface gravity, CNO abundances, and mass-loss rates. Finally, we compared the derived metalabundances with prediction from Geneva stellar evolution models. The frequency spectra of all threestars show stochastic oscillations and indications of one nonradial strange mode, fr = 0.09321 d−1inHD 42087 and a rotational splitting centred in f2 = 0.36366 d−1in HD 52089. We conclude that therather short sectoral observing windows of TESS prevent establishing a reliable mode identificationof low frequencies connected to mass-loss variabilities. The spectral analysis confirmed gradualchanges in the mass-loss rates, and the derived CNO abundances comply with the values reportedin the literature. We were able to achieve a quantitative match with stellar evolution models for thestellar masses and luminosities. However, the spectroscopic surface abundances turned out to beinconsistent with the theoretical predictions. The stars show N enrichment, typical for CNO cycleprocessed material, but the abundance ratios did not reflect the associated levels of C and O depletion.We found HD 42087 to be the most consistent with a pre-RSG evolutionary stage, HD 58350 is mostlikely in a post-RSG evolution and HD 52089 shows stellar parameters compatible with a star atthe TAMS.
Fil: Sánchez Arias, Julieta Paz. Czech Academy of Sciences; República Checa. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Németh, Péter. Czech Academy of Sciences; República Checa
Fil: Saldanha da Gama de Almeida, Elisson. Universidad de Valparaíso; Chile
Fil: Ruiz Diaz, Matias Agustin. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Kraus, Michaela. Czech Academy of Sciences; República Checa
Fil: Haucke, Maximiliano. Universidad Nacional de La Plata; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
description We aim to combine asteroseismology, spectroscopy, and evolutionary models to establisha comprehensive picture of the evolution of Galactic blue supergiant stars (BSG). To start such aninvestigation, we selected three BSG candidates for our analysis: HD 42087 (PU Gem), HD 52089(e CMa), and HD 58350 (η CMa). These stars show pulsations and were suspected to be in anevolutionary stage either preceding or succeding the red supergiant (RSG) stage. For our analysis,we utilized the 2-min cadence TESS data to study the photometric variability, and we obtained newspectroscopic observations at the CASLEO observatory. We used non-LTE radiative transfer modelscalculated with CMFGEN to derive their stellar and wind parameters. For the fitting procedure,we included CMFGEN models in the iterative spectral analysis pipeline XTGRID to determine theirCNO abundances. The spectral modeling was limited to changing only the effective temperature,surface gravity, CNO abundances, and mass-loss rates. Finally, we compared the derived metalabundances with prediction from Geneva stellar evolution models. The frequency spectra of all threestars show stochastic oscillations and indications of one nonradial strange mode, fr = 0.09321 d−1inHD 42087 and a rotational splitting centred in f2 = 0.36366 d−1in HD 52089. We conclude that therather short sectoral observing windows of TESS prevent establishing a reliable mode identificationof low frequencies connected to mass-loss variabilities. The spectral analysis confirmed gradualchanges in the mass-loss rates, and the derived CNO abundances comply with the values reportedin the literature. We were able to achieve a quantitative match with stellar evolution models for thestellar masses and luminosities. However, the spectroscopic surface abundances turned out to beinconsistent with the theoretical predictions. The stars show N enrichment, typical for CNO cycleprocessed material, but the abundance ratios did not reflect the associated levels of C and O depletion.We found HD 42087 to be the most consistent with a pre-RSG evolutionary stage, HD 58350 is mostlikely in a post-RSG evolution and HD 52089 shows stellar parameters compatible with a star atthe TAMS.
publishDate 2023
dc.date.none.fl_str_mv 2023-08
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/236319
Sánchez Arias, Julieta Paz; Németh, Péter; Saldanha da Gama de Almeida, Elisson; Ruiz Diaz, Matias Agustin; Kraus, Michaela; et al.; Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMa; MDPI; Galaxies; 11; 5; 8-2023; 93-122
2075-4434
CONICET Digital
CONICET
url http://hdl.handle.net/11336/236319
identifier_str_mv Sánchez Arias, Julieta Paz; Németh, Péter; Saldanha da Gama de Almeida, Elisson; Ruiz Diaz, Matias Agustin; Kraus, Michaela; et al.; Unveiling the evolutionary state of three B supergiant stars: PU Gem, ϵ CMa, and η CMa; MDPI; Galaxies; 11; 5; 8-2023; 93-122
2075-4434
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://www.mdpi.com/2075-4434/11/5/93
info:eu-repo/semantics/altIdentifier/doi/10.3390/galaxies11050093
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv MDPI
publisher.none.fl_str_mv MDPI
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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