Omega -slow solutions and Be star disks

Autores
Araya, I.; Jones, C. E.; Curé, M.; Silaj, J.; Cidale, Lydia Sonia; Granada, A.; Jiménez, A.
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
As the disk formation mechanism(s) in Be stars is(are) as yet unknown, we investigate the role of rapidly rotating radiationdrivenwinds in this process. We implemented the effects of high stellar rotation on m-CAK models accounting for: the shape of the star, the oblate finite disk correction factor, and gravity darkening. For a fast rotating star, we obtain a two-component wind model, i.e., a fast, thin wind in the polar latitudes and an Ω-slow, dense wind in the equatorial regions. We use the equatorialmass densities to explore Hα emission profiles for the following scenarios: 1) a spherically symmetric star, 2) an oblate shaped star with constant temperature, and 3) an oblate star with gravity darkening. One result of this work is that we have developed a novel method for solving the gravity darkened, oblated m-CAK equation of motion. Furthermore, from our modeling we finda) the oblate finite disk correction factor, for the scenario considering the gravity darkening, can vary by at least a factor of two between the equatorial and polar directions, influencing the velocity profile and mass-loss rate accordingly, b) the Hα profiles predicted by our model are in agreement with those predicted by a standard power-law model for following values of the lineforce parameters: 1.5 . k . 3, α ∼ 0.6 and δ & 0.1, and c) the contribution of the fast wind component to the Hα emission line profile is negligible; therefore, the line profiles arise mainly from the equatorial disks of Be stars.
Fil: Araya, I.. Universidad de Valparaiso, Chile;
Fil: Jones, C. E.. University of Western Ontario; Canadá
Fil: Curé, M.. Universidad de Valparaiso, Chile;
Fil: Silaj, J.. University of Western Ontario; Canadá
Fil: Cidale, Lydia Sonia. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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
Fil: Granada, A.. 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. University of Western Ontario; Canadá
Fil: Jiménez, A.. Universidad de Valparaiso, Chile;
Materia
Circumstellar matter
Winds
Be stars
Emission lines
Hydrodynamics
Outflows
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:11336/35922

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network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Omega -slow solutions and Be star disksAraya, I.Jones, C. E.Curé, M.Silaj, J.Cidale, Lydia SoniaGranada, A.Jiménez, A.Circumstellar matterWindsBe starsEmission linesHydrodynamicsOutflowshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1As the disk formation mechanism(s) in Be stars is(are) as yet unknown, we investigate the role of rapidly rotating radiationdrivenwinds in this process. We implemented the effects of high stellar rotation on m-CAK models accounting for: the shape of the star, the oblate finite disk correction factor, and gravity darkening. For a fast rotating star, we obtain a two-component wind model, i.e., a fast, thin wind in the polar latitudes and an Ω-slow, dense wind in the equatorial regions. We use the equatorialmass densities to explore Hα emission profiles for the following scenarios: 1) a spherically symmetric star, 2) an oblate shaped star with constant temperature, and 3) an oblate star with gravity darkening. One result of this work is that we have developed a novel method for solving the gravity darkened, oblated m-CAK equation of motion. Furthermore, from our modeling we finda) the oblate finite disk correction factor, for the scenario considering the gravity darkening, can vary by at least a factor of two between the equatorial and polar directions, influencing the velocity profile and mass-loss rate accordingly, b) the Hα profiles predicted by our model are in agreement with those predicted by a standard power-law model for following values of the lineforce parameters: 1.5 . k . 3, α ∼ 0.6 and δ & 0.1, and c) the contribution of the fast wind component to the Hα emission line profile is negligible; therefore, the line profiles arise mainly from the equatorial disks of Be stars.Fil: Araya, I.. Universidad de Valparaiso, Chile;Fil: Jones, C. E.. University of Western Ontario; CanadáFil: Curé, M.. Universidad de Valparaiso, Chile;Fil: Silaj, J.. University of Western Ontario; CanadáFil: Cidale, Lydia Sonia. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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; ArgentinaFil: Granada, A.. 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. University of Western Ontario; CanadáFil: Jiménez, A.. Universidad de Valparaiso, Chile;IOP Publishing2017-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/35922Araya, I.; Jones, C. E.; Curé, M.; Silaj, J.; Cidale, Lydia Sonia; et al.; Omega -slow solutions and Be star disks; IOP Publishing; Astrophysical Journal; 846; 9-2017; 1-150004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/1538-4357/aa835e/pdfinfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa835einfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:40:33Zoai:ri.conicet.gov.ar:11336/35922instacron: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 09:40:33.414CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Omega -slow solutions and Be star disks
title Omega -slow solutions and Be star disks
spellingShingle Omega -slow solutions and Be star disks
Araya, I.
Circumstellar matter
Winds
Be stars
Emission lines
Hydrodynamics
Outflows
title_short Omega -slow solutions and Be star disks
title_full Omega -slow solutions and Be star disks
title_fullStr Omega -slow solutions and Be star disks
title_full_unstemmed Omega -slow solutions and Be star disks
title_sort Omega -slow solutions and Be star disks
dc.creator.none.fl_str_mv Araya, I.
Jones, C. E.
Curé, M.
Silaj, J.
Cidale, Lydia Sonia
Granada, A.
Jiménez, A.
author Araya, I.
author_facet Araya, I.
Jones, C. E.
Curé, M.
Silaj, J.
Cidale, Lydia Sonia
Granada, A.
Jiménez, A.
author_role author
author2 Jones, C. E.
Curé, M.
Silaj, J.
Cidale, Lydia Sonia
Granada, A.
Jiménez, A.
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv Circumstellar matter
Winds
Be stars
Emission lines
Hydrodynamics
Outflows
topic Circumstellar matter
Winds
Be stars
Emission lines
Hydrodynamics
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 As the disk formation mechanism(s) in Be stars is(are) as yet unknown, we investigate the role of rapidly rotating radiationdrivenwinds in this process. We implemented the effects of high stellar rotation on m-CAK models accounting for: the shape of the star, the oblate finite disk correction factor, and gravity darkening. For a fast rotating star, we obtain a two-component wind model, i.e., a fast, thin wind in the polar latitudes and an Ω-slow, dense wind in the equatorial regions. We use the equatorialmass densities to explore Hα emission profiles for the following scenarios: 1) a spherically symmetric star, 2) an oblate shaped star with constant temperature, and 3) an oblate star with gravity darkening. One result of this work is that we have developed a novel method for solving the gravity darkened, oblated m-CAK equation of motion. Furthermore, from our modeling we finda) the oblate finite disk correction factor, for the scenario considering the gravity darkening, can vary by at least a factor of two between the equatorial and polar directions, influencing the velocity profile and mass-loss rate accordingly, b) the Hα profiles predicted by our model are in agreement with those predicted by a standard power-law model for following values of the lineforce parameters: 1.5 . k . 3, α ∼ 0.6 and δ & 0.1, and c) the contribution of the fast wind component to the Hα emission line profile is negligible; therefore, the line profiles arise mainly from the equatorial disks of Be stars.
Fil: Araya, I.. Universidad de Valparaiso, Chile;
Fil: Jones, C. E.. University of Western Ontario; Canadá
Fil: Curé, M.. Universidad de Valparaiso, Chile;
Fil: Silaj, J.. University of Western Ontario; Canadá
Fil: Cidale, Lydia Sonia. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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
Fil: Granada, A.. 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. University of Western Ontario; Canadá
Fil: Jiménez, A.. Universidad de Valparaiso, Chile;
description As the disk formation mechanism(s) in Be stars is(are) as yet unknown, we investigate the role of rapidly rotating radiationdrivenwinds in this process. We implemented the effects of high stellar rotation on m-CAK models accounting for: the shape of the star, the oblate finite disk correction factor, and gravity darkening. For a fast rotating star, we obtain a two-component wind model, i.e., a fast, thin wind in the polar latitudes and an Ω-slow, dense wind in the equatorial regions. We use the equatorialmass densities to explore Hα emission profiles for the following scenarios: 1) a spherically symmetric star, 2) an oblate shaped star with constant temperature, and 3) an oblate star with gravity darkening. One result of this work is that we have developed a novel method for solving the gravity darkened, oblated m-CAK equation of motion. Furthermore, from our modeling we finda) the oblate finite disk correction factor, for the scenario considering the gravity darkening, can vary by at least a factor of two between the equatorial and polar directions, influencing the velocity profile and mass-loss rate accordingly, b) the Hα profiles predicted by our model are in agreement with those predicted by a standard power-law model for following values of the lineforce parameters: 1.5 . k . 3, α ∼ 0.6 and δ & 0.1, and c) the contribution of the fast wind component to the Hα emission line profile is negligible; therefore, the line profiles arise mainly from the equatorial disks of Be stars.
publishDate 2017
dc.date.none.fl_str_mv 2017-09
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/11336/35922
Araya, I.; Jones, C. E.; Curé, M.; Silaj, J.; Cidale, Lydia Sonia; et al.; Omega -slow solutions and Be star disks; IOP Publishing; Astrophysical Journal; 846; 9-2017; 1-15
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/35922
identifier_str_mv Araya, I.; Jones, C. E.; Curé, M.; Silaj, J.; Cidale, Lydia Sonia; et al.; Omega -slow solutions and Be star disks; IOP Publishing; Astrophysical Journal; 846; 9-2017; 1-15
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/10.3847/1538-4357/aa835e/pdf
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa835e
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 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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