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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/262926
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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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1846781938284625920 |
score |
12.982451 |