Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars

Autores
Araya, I.; Curé, M.; ud-Doula, A.; Santillán, A.; Cidale, Lydia Sonia
Año de publicación
2018
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Most radiation-driven winds of massive stars can be modelled with m-CAK theory, resulting in the so-called fast solution. However, the most rapidly rotating stars among them, especially when the rotational speed is higher than ~75 per cent of the critical rotational speed, can adopt a different solution, the so-called Ω-slow solution, characterized by a dense and slow wind. Here, we study the transition region of the solutions where the fast solution changes to the Ω-slow solution. Using both time-steady and time-dependent numerical codes, we study this transition region for various equatorial models of B-type stars. In all cases, in a certain range of rotational speeds we find a region where the fast and the Ω-slow solution can coexist. We find that the type of solution obtained in this co-existence region depends stongly on the initial conditions of our models. We also test the stability of the solutions within the co-existence region by performing base-density perturbations in the wind. We find that under certain conditions, the fast solution can switch to the Ω-slow solution, or vice versa. Such solution-switching may be a possible contributor of material injected into the circumstellar environment of Be stars, without requiring rotational speeds near critical values.
Fil: Araya, I.. Universidad Mayor; Chile. Universidad de Valparaiso; Chile
Fil: Curé, M.. Universidad de Valparaiso; Chile
Fil: ud-Doula, A.. Université de Liège; Bélgica. Pennsylvania State University;
Fil: Santillán, A.. Universidad Nacional Autónoma de México; México
Fil: Cidale, Lydia Sonia. Universidad de Valparaiso; Chile. 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
HYDRODYNAMICS
OUTFLOWS
STARS: EARLY-TYPE
STARS: ROTATION
STARS: WINDS
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/82696
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/82696
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive starsAraya, I.Curé, M.ud-Doula, A.Santillán, A.Cidale, Lydia SoniaHYDRODYNAMICSOUTFLOWSSTARS: EARLY-TYPESTARS: ROTATIONSTARS: WINDShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Most radiation-driven winds of massive stars can be modelled with m-CAK theory, resulting in the so-called fast solution. However, the most rapidly rotating stars among them, especially when the rotational speed is higher than ~75 per cent of the critical rotational speed, can adopt a different solution, the so-called Ω-slow solution, characterized by a dense and slow wind. Here, we study the transition region of the solutions where the fast solution changes to the Ω-slow solution. Using both time-steady and time-dependent numerical codes, we study this transition region for various equatorial models of B-type stars. In all cases, in a certain range of rotational speeds we find a region where the fast and the Ω-slow solution can coexist. We find that the type of solution obtained in this co-existence region depends stongly on the initial conditions of our models. We also test the stability of the solutions within the co-existence region by performing base-density perturbations in the wind. We find that under certain conditions, the fast solution can switch to the Ω-slow solution, or vice versa. Such solution-switching may be a possible contributor of material injected into the circumstellar environment of Be stars, without requiring rotational speeds near critical values.Fil: Araya, I.. Universidad Mayor; Chile. Universidad de Valparaiso; ChileFil: Curé, M.. Universidad de Valparaiso; ChileFil: ud-Doula, A.. Université de Liège; Bélgica. Pennsylvania State University;Fil: Santillán, A.. Universidad Nacional Autónoma de México; MéxicoFil: Cidale, Lydia Sonia. Universidad de Valparaiso; Chile. 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; ArgentinaWiley Blackwell Publishing, Inc2018-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/82696Araya, I.; Curé, M.; ud-Doula, A.; Santillán, A.; Cidale, Lydia Sonia; Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 477; 1; 4-2018; 755-7650035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sty678info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/477/1/755/4975263info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:03:58Zoai:ri.conicet.gov.ar:11336/82696instacron: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 11:03:58.757CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
title Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
spellingShingle Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
Araya, I.
HYDRODYNAMICS
OUTFLOWS
STARS: EARLY-TYPE
STARS: ROTATION
STARS: WINDS
title_short Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
title_full Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
title_fullStr Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
title_full_unstemmed Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
title_sort Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
dc.creator.none.fl_str_mv Araya, I.
Curé, M.
ud-Doula, A.
Santillán, A.
Cidale, Lydia Sonia
author Araya, I.
author_facet Araya, I.
Curé, M.
ud-Doula, A.
Santillán, A.
Cidale, Lydia Sonia
author_role author
author2 Curé, M.
ud-Doula, A.
Santillán, A.
Cidale, Lydia Sonia
author2_role author
author
author
author
dc.subject.none.fl_str_mv HYDRODYNAMICS
OUTFLOWS
STARS: EARLY-TYPE
STARS: ROTATION
STARS: WINDS
topic HYDRODYNAMICS
OUTFLOWS
STARS: EARLY-TYPE
STARS: ROTATION
STARS: 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 Most radiation-driven winds of massive stars can be modelled with m-CAK theory, resulting in the so-called fast solution. However, the most rapidly rotating stars among them, especially when the rotational speed is higher than ~75 per cent of the critical rotational speed, can adopt a different solution, the so-called Ω-slow solution, characterized by a dense and slow wind. Here, we study the transition region of the solutions where the fast solution changes to the Ω-slow solution. Using both time-steady and time-dependent numerical codes, we study this transition region for various equatorial models of B-type stars. In all cases, in a certain range of rotational speeds we find a region where the fast and the Ω-slow solution can coexist. We find that the type of solution obtained in this co-existence region depends stongly on the initial conditions of our models. We also test the stability of the solutions within the co-existence region by performing base-density perturbations in the wind. We find that under certain conditions, the fast solution can switch to the Ω-slow solution, or vice versa. Such solution-switching may be a possible contributor of material injected into the circumstellar environment of Be stars, without requiring rotational speeds near critical values.
Fil: Araya, I.. Universidad Mayor; Chile. Universidad de Valparaiso; Chile
Fil: Curé, M.. Universidad de Valparaiso; Chile
Fil: ud-Doula, A.. Université de Liège; Bélgica. Pennsylvania State University;
Fil: Santillán, A.. Universidad Nacional Autónoma de México; México
Fil: Cidale, Lydia Sonia. Universidad de Valparaiso; Chile. 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 Most radiation-driven winds of massive stars can be modelled with m-CAK theory, resulting in the so-called fast solution. However, the most rapidly rotating stars among them, especially when the rotational speed is higher than ~75 per cent of the critical rotational speed, can adopt a different solution, the so-called Ω-slow solution, characterized by a dense and slow wind. Here, we study the transition region of the solutions where the fast solution changes to the Ω-slow solution. Using both time-steady and time-dependent numerical codes, we study this transition region for various equatorial models of B-type stars. In all cases, in a certain range of rotational speeds we find a region where the fast and the Ω-slow solution can coexist. We find that the type of solution obtained in this co-existence region depends stongly on the initial conditions of our models. We also test the stability of the solutions within the co-existence region by performing base-density perturbations in the wind. We find that under certain conditions, the fast solution can switch to the Ω-slow solution, or vice versa. Such solution-switching may be a possible contributor of material injected into the circumstellar environment of Be stars, without requiring rotational speeds near critical values.
publishDate 2018
dc.date.none.fl_str_mv 2018-04
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/11336/82696
Araya, I.; Curé, M.; ud-Doula, A.; Santillán, A.; Cidale, Lydia Sonia; Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 477; 1; 4-2018; 755-765
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/82696
identifier_str_mv Araya, I.; Curé, M.; ud-Doula, A.; Santillán, A.; Cidale, Lydia Sonia; Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 477; 1; 4-2018; 755-765
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/doi/10.1093/mnras/sty678
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/477/1/755/4975263
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
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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