The wind of rotating B supergiants, I : domains of slow and fast solution regimes
- Autores
- Venero, Roberto Oscar José; Curé, M.; Cidale, Lydia Sonia; Araya, I.
- Año de publicación
- 2016
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- In the scenario of rotating radiation-driven wind theory for massive stars, three types of stationary hydrodynamic solutions are currently known: the classical ( fast) m-CAK solution, the Ω-slow solution that arises for fast rotators, and the so-called δ-slow solution if high values of the δ line-force parameter are allowed independently of the rotation speed. Compared to the fast solution, both ?slow solutions? have lower terminal velocities. As the study ofthe parameter domain for the slow solution is still incomplete, we perform a comprehensive analysis of the distinctive flow regimes for B supergiants that emerge from a fine grid of rotation values, Ω, and various ionizationconditions in the wind (δ) parameter. The wind ionization defines two domains: one for fast outflowing winds and the other for slow expanding flows. Both domains are clear-cut by a gap, where a kink/plateau structure of thevelocity law could exist for a finite interval of δ. The location and width of the gap depend on Teff and Ω. There is a smooth and continuous transition between the Ω-slow and δ-slow regimes, a single Ω δ-slow regime. We discussdifferent situations where the slow solutions can be found and the possibility of a switch between fast and slow solutions in B supergiant winds. We compare the theoretical terminal velocity with observations of B and Asupergiants and find that the fast regime prevails mostly for early B supergiants while the slow wind regime matches better for A and B mid- and late-type supergiants.
Fil: Venero, Roberto Oscar José. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Curé, M.. Universidad de Valparaíso; Chile
Fil: Cidale, Lydia Sonia. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Araya, I.. Universidad de Valparaíso; Chile - Materia
-
Hydrodynamics
Early type stars
Mass loss
Winds
Outflows
Stars: early-type
Stars: mass-loss - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/36434
Ver los metadatos del registro completo
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The wind of rotating B supergiants, I : domains of slow and fast solution regimesVenero, Roberto Oscar JoséCuré, M.Cidale, Lydia SoniaAraya, I.HydrodynamicsEarly type starsMass lossWindsOutflowsStars: early-typeStars: mass-losshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1In the scenario of rotating radiation-driven wind theory for massive stars, three types of stationary hydrodynamic solutions are currently known: the classical ( fast) m-CAK solution, the Ω-slow solution that arises for fast rotators, and the so-called δ-slow solution if high values of the δ line-force parameter are allowed independently of the rotation speed. Compared to the fast solution, both ?slow solutions? have lower terminal velocities. As the study ofthe parameter domain for the slow solution is still incomplete, we perform a comprehensive analysis of the distinctive flow regimes for B supergiants that emerge from a fine grid of rotation values, Ω, and various ionizationconditions in the wind (δ) parameter. The wind ionization defines two domains: one for fast outflowing winds and the other for slow expanding flows. Both domains are clear-cut by a gap, where a kink/plateau structure of thevelocity law could exist for a finite interval of δ. The location and width of the gap depend on Teff and Ω. There is a smooth and continuous transition between the Ω-slow and δ-slow regimes, a single Ω δ-slow regime. We discussdifferent situations where the slow solutions can be found and the possibility of a switch between fast and slow solutions in B supergiant winds. We compare the theoretical terminal velocity with observations of B and Asupergiants and find that the fast regime prevails mostly for early B supergiants while the slow wind regime matches better for A and B mid- and late-type supergiants.Fil: Venero, Roberto Oscar José. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Curé, M.. Universidad de Valparaíso; ChileFil: Cidale, Lydia Sonia. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Araya, I.. Universidad de Valparaíso; ChileIOP Publishing2016-05info: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/11336/36434Venero, Roberto Oscar José; Curé, M.; Cidale, Lydia Sonia; Araya, I.; The wind of rotating B supergiants, I : domains of slow and fast solution regimes; IOP Publishing; Astrophysical Journal; 822; 28; 5-2016; 1-110004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/0004-637X/822/1/28/pdfinfo:eu-repo/semantics/altIdentifier/doi/10.3847/0004-637X/822/1/28info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:51:20Zoai:ri.conicet.gov.ar:11336/36434instacron: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:34982025-09-29 09:51:21.061CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
The wind of rotating B supergiants, I : domains of slow and fast solution regimes |
title |
The wind of rotating B supergiants, I : domains of slow and fast solution regimes |
spellingShingle |
The wind of rotating B supergiants, I : domains of slow and fast solution regimes Venero, Roberto Oscar José Hydrodynamics Early type stars Mass loss Winds Outflows Stars: early-type Stars: mass-loss |
title_short |
The wind of rotating B supergiants, I : domains of slow and fast solution regimes |
title_full |
The wind of rotating B supergiants, I : domains of slow and fast solution regimes |
title_fullStr |
The wind of rotating B supergiants, I : domains of slow and fast solution regimes |
title_full_unstemmed |
The wind of rotating B supergiants, I : domains of slow and fast solution regimes |
title_sort |
The wind of rotating B supergiants, I : domains of slow and fast solution regimes |
dc.creator.none.fl_str_mv |
Venero, Roberto Oscar José Curé, M. Cidale, Lydia Sonia Araya, I. |
author |
Venero, Roberto Oscar José |
author_facet |
Venero, Roberto Oscar José Curé, M. Cidale, Lydia Sonia Araya, I. |
author_role |
author |
author2 |
Curé, M. Cidale, Lydia Sonia Araya, I. |
author2_role |
author author author |
dc.subject.none.fl_str_mv |
Hydrodynamics Early type stars Mass loss Winds Outflows Stars: early-type Stars: mass-loss |
topic |
Hydrodynamics Early type stars Mass loss Winds Outflows Stars: early-type Stars: mass-loss |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
In the scenario of rotating radiation-driven wind theory for massive stars, three types of stationary hydrodynamic solutions are currently known: the classical ( fast) m-CAK solution, the Ω-slow solution that arises for fast rotators, and the so-called δ-slow solution if high values of the δ line-force parameter are allowed independently of the rotation speed. Compared to the fast solution, both ?slow solutions? have lower terminal velocities. As the study ofthe parameter domain for the slow solution is still incomplete, we perform a comprehensive analysis of the distinctive flow regimes for B supergiants that emerge from a fine grid of rotation values, Ω, and various ionizationconditions in the wind (δ) parameter. The wind ionization defines two domains: one for fast outflowing winds and the other for slow expanding flows. Both domains are clear-cut by a gap, where a kink/plateau structure of thevelocity law could exist for a finite interval of δ. The location and width of the gap depend on Teff and Ω. There is a smooth and continuous transition between the Ω-slow and δ-slow regimes, a single Ω δ-slow regime. We discussdifferent situations where the slow solutions can be found and the possibility of a switch between fast and slow solutions in B supergiant winds. We compare the theoretical terminal velocity with observations of B and Asupergiants and find that the fast regime prevails mostly for early B supergiants while the slow wind regime matches better for A and B mid- and late-type supergiants. Fil: Venero, Roberto Oscar José. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Curé, M.. Universidad de Valparaíso; Chile Fil: Cidale, Lydia Sonia. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Araya, I.. Universidad de Valparaíso; Chile |
description |
In the scenario of rotating radiation-driven wind theory for massive stars, three types of stationary hydrodynamic solutions are currently known: the classical ( fast) m-CAK solution, the Ω-slow solution that arises for fast rotators, and the so-called δ-slow solution if high values of the δ line-force parameter are allowed independently of the rotation speed. Compared to the fast solution, both ?slow solutions? have lower terminal velocities. As the study ofthe parameter domain for the slow solution is still incomplete, we perform a comprehensive analysis of the distinctive flow regimes for B supergiants that emerge from a fine grid of rotation values, Ω, and various ionizationconditions in the wind (δ) parameter. The wind ionization defines two domains: one for fast outflowing winds and the other for slow expanding flows. Both domains are clear-cut by a gap, where a kink/plateau structure of thevelocity law could exist for a finite interval of δ. The location and width of the gap depend on Teff and Ω. There is a smooth and continuous transition between the Ω-slow and δ-slow regimes, a single Ω δ-slow regime. We discussdifferent situations where the slow solutions can be found and the possibility of a switch between fast and slow solutions in B supergiant winds. We compare the theoretical terminal velocity with observations of B and Asupergiants and find that the fast regime prevails mostly for early B supergiants while the slow wind regime matches better for A and B mid- and late-type supergiants. |
publishDate |
2016 |
dc.date.none.fl_str_mv |
2016-05 |
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/11336/36434 Venero, Roberto Oscar José; Curé, M.; Cidale, Lydia Sonia; Araya, I.; The wind of rotating B supergiants, I : domains of slow and fast solution regimes; IOP Publishing; Astrophysical Journal; 822; 28; 5-2016; 1-11 0004-637X CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/36434 |
identifier_str_mv |
Venero, Roberto Oscar José; Curé, M.; Cidale, Lydia Sonia; Araya, I.; The wind of rotating B supergiants, I : domains of slow and fast solution regimes; IOP Publishing; Astrophysical Journal; 822; 28; 5-2016; 1-11 0004-637X CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/0004-637X/822/1/28/pdf info:eu-repo/semantics/altIdentifier/doi/10.3847/0004-637X/822/1/28 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
IOP Publishing |
publisher.none.fl_str_mv |
IOP Publishing |
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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1844613578725785600 |
score |
13.070432 |