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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/222918
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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 Técnicas2025-09-29T10:35:37Zoai: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:34982025-09-29 10:35:37.533CONICET 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 |
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1844614375106674688 |
score |
13.070432 |