The wind of rotating B supergiants – II: The δ-slow hydrodynamic regime

Autores
Venero, Roberto Oscar José; Curé, M.; Puls, J.; Cidale, Lydia Sonia; Haucke, Maximiliano; Araya, Teresa Ivana; Gormaz Matamala, A.; Arcos, C.
Año de publicación
2024
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The theory of line-driven winds can explain many observed spectral features in early-type stars, though our understanding the winds of B supergiants remains incomplete. The hydrodynamic equations for slowly rotating stellar winds predict two regimes based on the line-force parameter δ: the fast and the δ-slow solution. In this paper, we aim to explore the capability of the latter to explain the observed properties of B supergiant winds. We calculate Hα line profiles, the most sensitive wind diagnostics in the optical, for both fast and δ-slow wind models. We fit them to observed data from a well-studied sample of B supergiants, by adapting the line-force parameters (k, α, and δ) of the hydrodynamic model. Unexpectedly, the observed Hα spectra can be reproduced by both hydrodynamic wind regimes with similar precision. We argue that this similarity results from the similar shape of the normalized velocity law produced by both regimes in the lower, Hα-forming wind region. Our findings raise a dichotomy, because mass-loss rates and terminal velocities (v∞) for each solution are quite different. The δ-slow solution predicts maximum values for v∞ that are systematically lower than those measured in the ultraviolet, whereas the v∞ values of the fast solution are closer, and probably more appropriate. However, our results also indicate that the δ-slow solution might better describe the dense winds of B hypergiants. Multiwavelength analyses and a larger sample of stars are needed to reach a definitive conclusion.
Fil: Venero, Roberto Oscar José. 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. Universidad Nacional de la Plata. Facultad de Cs.astronómicas y Geofísicas. Departamento de Espectrocopia Estelar; Argentina
Fil: Curé, M.. Universidad de Valparaíso; Chile
Fil: Puls, J.. Ludwig Maximilians Universitat; Alemania
Fil: Cidale, Lydia Sonia. 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. Universidad Nacional de la Plata. Facultad de Cs.astronómicas y Geofísicas. Departamento de Espectrocopia Estelar; Argentina
Fil: Haucke, Maximiliano. 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. Universidad Nacional de La Plata. Facultad de Ingeniería; Argentina
Fil: Araya, Teresa Ivana. Universidad Mayor.; Chile
Fil: Gormaz Matamala, A.. Universidad Adolfo Ibañez; Chile. Polish Academy of Sciences; Argentina. Pontificia Universidad Católica de Chile; Chile
Fil: Arcos, C.. Universidad de Valparaíso; Chile
Materia
Hydrodynamics
Stars: early-type
Stars: mass-loss
Stars: winds, outflows
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:11336/262926
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/262926
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The wind of rotating B supergiants – II: The δ-slow hydrodynamic regimeVenero, Roberto Oscar JoséCuré, M.Puls, J.Cidale, Lydia SoniaHaucke, MaximilianoAraya, Teresa IvanaGormaz Matamala, A.Arcos, C.HydrodynamicsStars: early-typeStars: mass-lossStars: winds, outflowshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The theory of line-driven winds can explain many observed spectral features in early-type stars, though our understanding the winds of B supergiants remains incomplete. The hydrodynamic equations for slowly rotating stellar winds predict two regimes based on the line-force parameter δ: the fast and the δ-slow solution. In this paper, we aim to explore the capability of the latter to explain the observed properties of B supergiant winds. We calculate Hα line profiles, the most sensitive wind diagnostics in the optical, for both fast and δ-slow wind models. We fit them to observed data from a well-studied sample of B supergiants, by adapting the line-force parameters (k, α, and δ) of the hydrodynamic model. Unexpectedly, the observed Hα spectra can be reproduced by both hydrodynamic wind regimes with similar precision. We argue that this similarity results from the similar shape of the normalized velocity law produced by both regimes in the lower, Hα-forming wind region. Our findings raise a dichotomy, because mass-loss rates and terminal velocities (v∞) for each solution are quite different. The δ-slow solution predicts maximum values for v∞ that are systematically lower than those measured in the ultraviolet, whereas the v∞ values of the fast solution are closer, and probably more appropriate. However, our results also indicate that the δ-slow solution might better describe the dense winds of B hypergiants. Multiwavelength analyses and a larger sample of stars are needed to reach a definitive conclusion.Fil: Venero, Roberto Oscar José. 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. Universidad Nacional de la Plata. Facultad de Cs.astronómicas y Geofísicas. Departamento de Espectrocopia Estelar; ArgentinaFil: Curé, M.. Universidad de Valparaíso; ChileFil: Puls, J.. Ludwig Maximilians Universitat; AlemaniaFil: Cidale, Lydia Sonia. 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. Universidad Nacional de la Plata. Facultad de Cs.astronómicas y Geofísicas. Departamento de Espectrocopia Estelar; ArgentinaFil: Haucke, Maximiliano. 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. Universidad Nacional de La Plata. Facultad de Ingeniería; ArgentinaFil: Araya, Teresa Ivana. Universidad Mayor.; ChileFil: Gormaz Matamala, A.. Universidad Adolfo Ibañez; Chile. Polish Academy of Sciences; Argentina. Pontificia Universidad Católica de Chile; ChileFil: Arcos, C.. Universidad de Valparaíso; ChileWiley Blackwell Publishing, Inc2024-01info: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/11336/262926Venero, Roberto Oscar José; Curé, M.; Puls, J.; Cidale, Lydia Sonia; Haucke, Maximiliano; et al.; The wind of rotating B supergiants – II: The δ-slow hydrodynamic regime; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 527; 1; 1-2024; 93-1110035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/527/1/93/7379781info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stad3030info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:32:37Zoai:ri.conicet.gov.ar:11336/262926instacron: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 11:32:37.423CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The wind of rotating B supergiants – II: The δ-slow hydrodynamic regime
title The wind of rotating B supergiants – II: The δ-slow hydrodynamic regime
spellingShingle The wind of rotating B supergiants – II: The δ-slow hydrodynamic regime
Venero, Roberto Oscar José
Hydrodynamics
Stars: early-type
Stars: mass-loss
Stars: winds, outflows
title_short The wind of rotating B supergiants – II: The δ-slow hydrodynamic regime
title_full The wind of rotating B supergiants – II: The δ-slow hydrodynamic regime
title_fullStr The wind of rotating B supergiants – II: The δ-slow hydrodynamic regime
title_full_unstemmed The wind of rotating B supergiants – II: The δ-slow hydrodynamic regime
title_sort The wind of rotating B supergiants – II: The δ-slow hydrodynamic regime
dc.creator.none.fl_str_mv Venero, Roberto Oscar José
Curé, M.
Puls, J.
Cidale, Lydia Sonia
Haucke, Maximiliano
Araya, Teresa Ivana
Gormaz Matamala, A.
Arcos, C.
author Venero, Roberto Oscar José
author_facet Venero, Roberto Oscar José
Curé, M.
Puls, J.
Cidale, Lydia Sonia
Haucke, Maximiliano
Araya, Teresa Ivana
Gormaz Matamala, A.
Arcos, C.
author_role author
author2 Curé, M.
Puls, J.
Cidale, Lydia Sonia
Haucke, Maximiliano
Araya, Teresa Ivana
Gormaz Matamala, A.
Arcos, C.
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Hydrodynamics
Stars: early-type
Stars: mass-loss
Stars: winds, outflows
topic Hydrodynamics
Stars: early-type
Stars: mass-loss
Stars: winds, outflows
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The theory of line-driven winds can explain many observed spectral features in early-type stars, though our understanding the winds of B supergiants remains incomplete. The hydrodynamic equations for slowly rotating stellar winds predict two regimes based on the line-force parameter δ: the fast and the δ-slow solution. In this paper, we aim to explore the capability of the latter to explain the observed properties of B supergiant winds. We calculate Hα line profiles, the most sensitive wind diagnostics in the optical, for both fast and δ-slow wind models. We fit them to observed data from a well-studied sample of B supergiants, by adapting the line-force parameters (k, α, and δ) of the hydrodynamic model. Unexpectedly, the observed Hα spectra can be reproduced by both hydrodynamic wind regimes with similar precision. We argue that this similarity results from the similar shape of the normalized velocity law produced by both regimes in the lower, Hα-forming wind region. Our findings raise a dichotomy, because mass-loss rates and terminal velocities (v∞) for each solution are quite different. The δ-slow solution predicts maximum values for v∞ that are systematically lower than those measured in the ultraviolet, whereas the v∞ values of the fast solution are closer, and probably more appropriate. However, our results also indicate that the δ-slow solution might better describe the dense winds of B hypergiants. Multiwavelength analyses and a larger sample of stars are needed to reach a definitive conclusion.
Fil: Venero, Roberto Oscar José. 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. Universidad Nacional de la Plata. Facultad de Cs.astronómicas y Geofísicas. Departamento de Espectrocopia Estelar; Argentina
Fil: Curé, M.. Universidad de Valparaíso; Chile
Fil: Puls, J.. Ludwig Maximilians Universitat; Alemania
Fil: Cidale, Lydia Sonia. 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. Universidad Nacional de la Plata. Facultad de Cs.astronómicas y Geofísicas. Departamento de Espectrocopia Estelar; Argentina
Fil: Haucke, Maximiliano. 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. Universidad Nacional de La Plata. Facultad de Ingeniería; Argentina
Fil: Araya, Teresa Ivana. Universidad Mayor.; Chile
Fil: Gormaz Matamala, A.. Universidad Adolfo Ibañez; Chile. Polish Academy of Sciences; Argentina. Pontificia Universidad Católica de Chile; Chile
Fil: Arcos, C.. Universidad de Valparaíso; Chile
description The theory of line-driven winds can explain many observed spectral features in early-type stars, though our understanding the winds of B supergiants remains incomplete. The hydrodynamic equations for slowly rotating stellar winds predict two regimes based on the line-force parameter δ: the fast and the δ-slow solution. In this paper, we aim to explore the capability of the latter to explain the observed properties of B supergiant winds. We calculate Hα line profiles, the most sensitive wind diagnostics in the optical, for both fast and δ-slow wind models. We fit them to observed data from a well-studied sample of B supergiants, by adapting the line-force parameters (k, α, and δ) of the hydrodynamic model. Unexpectedly, the observed Hα spectra can be reproduced by both hydrodynamic wind regimes with similar precision. We argue that this similarity results from the similar shape of the normalized velocity law produced by both regimes in the lower, Hα-forming wind region. Our findings raise a dichotomy, because mass-loss rates and terminal velocities (v∞) for each solution are quite different. The δ-slow solution predicts maximum values for v∞ that are systematically lower than those measured in the ultraviolet, whereas the v∞ values of the fast solution are closer, and probably more appropriate. However, our results also indicate that the δ-slow solution might better describe the dense winds of B hypergiants. Multiwavelength analyses and a larger sample of stars are needed to reach a definitive conclusion.
publishDate 2024
dc.date.none.fl_str_mv 2024-01
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/11336/262926
Venero, Roberto Oscar José; Curé, M.; Puls, J.; Cidale, Lydia Sonia; Haucke, Maximiliano; et al.; The wind of rotating B supergiants – II: The δ-slow hydrodynamic regime; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 527; 1; 1-2024; 93-111
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/262926
identifier_str_mv Venero, Roberto Oscar José; Curé, M.; Puls, J.; Cidale, Lydia Sonia; Haucke, Maximiliano; et al.; The wind of rotating B supergiants – II: The δ-slow hydrodynamic regime; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 527; 1; 1-2024; 93-111
0035-8711
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://academic.oup.com/mnras/article/527/1/93/7379781
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stad3030
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 Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
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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score 12.982451

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