Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc model

Autores
Ghoreyshi, M. R.; Jones, C. E.; Granada, Anahi
Año de publicación
2023
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Circumstellar discs around Be stars are formed by the material ejected by the central star. This process removes excess angular momentum from the star as viscosity facilitates the mass and angular momentum transfer within the disc and its growth. The angular momentum loss rates (AMLR) of Be stars is a subject of debate in the literature. Through the modelling of the disc formation and dissipation phases observed from Be stars, their average AMLR can be determined and this is the goal of this work. We use the viscous decretion disc (VDD) model to provide a range of the average AMLR for Be stars and compare these rates with predicted values from the literature. We explore the reasons for discrepancies between the predicted values of average AMLR, using the VDD and Geneva stellar evolution models that were previously reported in literature and find that the largest differences occur when Be stars are rotating below their critical speeds. We show that the time over which the mass reservoir builds up is inversely proportional to the average AMLR. Also, we determine a revised value of the average AMLR for the Galactic Be star ω CMa of 4.7× 1036g, cm2, s-2, which is in better agreement with the values expected for a typical B2-type star. Finally, the effect of disc truncation due to the presence of a companion star is investigated and we find that this has a minimal effect on the average AMLR.
Fil: Ghoreyshi, M. R.. Western University; Canadá
Fil: Jones, C. E.. Western University; Canadá
Fil: Granada, Anahi. Universidad Nacional de Río Negro. Sede Andina; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Patagonia Norte; Argentina
Materia
STARS: EMISSION-LINE, BE
STARS: INDIVIDUAL: Ω CMA
STARS: MASS-LOSS
STARS: MASSIVE
STARS: ROTATION
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:11336/222918
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/222918
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc modelGhoreyshi, M. R.Jones, C. E.Granada, AnahiSTARS: EMISSION-LINE, BESTARS: INDIVIDUAL: Ω CMASTARS: MASS-LOSSSTARS: MASSIVESTARS: ROTATIONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Circumstellar discs around Be stars are formed by the material ejected by the central star. This process removes excess angular momentum from the star as viscosity facilitates the mass and angular momentum transfer within the disc and its growth. The angular momentum loss rates (AMLR) of Be stars is a subject of debate in the literature. Through the modelling of the disc formation and dissipation phases observed from Be stars, their average AMLR can be determined and this is the goal of this work. We use the viscous decretion disc (VDD) model to provide a range of the average AMLR for Be stars and compare these rates with predicted values from the literature. We explore the reasons for discrepancies between the predicted values of average AMLR, using the VDD and Geneva stellar evolution models that were previously reported in literature and find that the largest differences occur when Be stars are rotating below their critical speeds. We show that the time over which the mass reservoir builds up is inversely proportional to the average AMLR. Also, we determine a revised value of the average AMLR for the Galactic Be star ω CMa of 4.7× 1036g, cm2, s-2, which is in better agreement with the values expected for a typical B2-type star. Finally, the effect of disc truncation due to the presence of a companion star is investigated and we find that this has a minimal effect on the average AMLR.Fil: Ghoreyshi, M. R.. Western University; CanadáFil: Jones, C. E.. Western University; CanadáFil: Granada, Anahi. Universidad Nacional de Río Negro. Sede Andina; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Patagonia Norte; ArgentinaWiley Blackwell Publishing, Inc2023-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/222918Ghoreyshi, M. R.; Jones, C. E.; Granada, Anahi; Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc model; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 518; 1; 1-2023; 30-380035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stac3084info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T12:07:56Zoai:ri.conicet.gov.ar:11336/222918instacron: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 12:07:57.226CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc model
title Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc model
spellingShingle Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc model
Ghoreyshi, M. R.
STARS: EMISSION-LINE, BE
STARS: INDIVIDUAL: Ω CMA
STARS: MASS-LOSS
STARS: MASSIVE
STARS: ROTATION
title_short Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc model
title_full Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc model
title_fullStr Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc model
title_full_unstemmed Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc model
title_sort Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc model
dc.creator.none.fl_str_mv Ghoreyshi, M. R.
Jones, C. E.
Granada, Anahi
author Ghoreyshi, M. R.
author_facet Ghoreyshi, M. R.
Jones, C. E.
Granada, Anahi
author_role author
author2 Jones, C. E.
Granada, Anahi
author2_role author
author
dc.subject.none.fl_str_mv STARS: EMISSION-LINE, BE
STARS: INDIVIDUAL: Ω CMA
STARS: MASS-LOSS
STARS: MASSIVE
STARS: ROTATION
topic STARS: EMISSION-LINE, BE
STARS: INDIVIDUAL: Ω CMA
STARS: MASS-LOSS
STARS: MASSIVE
STARS: ROTATION
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Circumstellar discs around Be stars are formed by the material ejected by the central star. This process removes excess angular momentum from the star as viscosity facilitates the mass and angular momentum transfer within the disc and its growth. The angular momentum loss rates (AMLR) of Be stars is a subject of debate in the literature. Through the modelling of the disc formation and dissipation phases observed from Be stars, their average AMLR can be determined and this is the goal of this work. We use the viscous decretion disc (VDD) model to provide a range of the average AMLR for Be stars and compare these rates with predicted values from the literature. We explore the reasons for discrepancies between the predicted values of average AMLR, using the VDD and Geneva stellar evolution models that were previously reported in literature and find that the largest differences occur when Be stars are rotating below their critical speeds. We show that the time over which the mass reservoir builds up is inversely proportional to the average AMLR. Also, we determine a revised value of the average AMLR for the Galactic Be star ω CMa of 4.7× 1036g, cm2, s-2, which is in better agreement with the values expected for a typical B2-type star. Finally, the effect of disc truncation due to the presence of a companion star is investigated and we find that this has a minimal effect on the average AMLR.
Fil: Ghoreyshi, M. R.. Western University; Canadá
Fil: Jones, C. E.. Western University; Canadá
Fil: Granada, Anahi. Universidad Nacional de Río Negro. Sede Andina; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Patagonia Norte; Argentina
description Circumstellar discs around Be stars are formed by the material ejected by the central star. This process removes excess angular momentum from the star as viscosity facilitates the mass and angular momentum transfer within the disc and its growth. The angular momentum loss rates (AMLR) of Be stars is a subject of debate in the literature. Through the modelling of the disc formation and dissipation phases observed from Be stars, their average AMLR can be determined and this is the goal of this work. We use the viscous decretion disc (VDD) model to provide a range of the average AMLR for Be stars and compare these rates with predicted values from the literature. We explore the reasons for discrepancies between the predicted values of average AMLR, using the VDD and Geneva stellar evolution models that were previously reported in literature and find that the largest differences occur when Be stars are rotating below their critical speeds. We show that the time over which the mass reservoir builds up is inversely proportional to the average AMLR. Also, we determine a revised value of the average AMLR for the Galactic Be star ω CMa of 4.7× 1036g, cm2, s-2, which is in better agreement with the values expected for a typical B2-type star. Finally, the effect of disc truncation due to the presence of a companion star is investigated and we find that this has a minimal effect on the average AMLR.
publishDate 2023
dc.date.none.fl_str_mv 2023-01
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/11336/222918
Ghoreyshi, M. R.; Jones, C. E.; Granada, Anahi; Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc model; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 518; 1; 1-2023; 30-38
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/222918
identifier_str_mv Ghoreyshi, M. R.; Jones, C. E.; Granada, Anahi; Angular Momentum Loss Rates in Be stars determined by the Viscous Decretion Disc model; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 518; 1; 1-2023; 30-38
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/stac3084
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
_version_ 1846782447730032640
score 12.982451

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