Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds

The effects of rapid rotation and bi-stability upon the density contrast between the equatorial and polar directions of a B[e] supergiant are re-investigated. Based on a new slow solution for different high rotational radiation-driven winds and the fact that bi-stability allows a cha...

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Autores principales: Curé, M., Rial, D.F., Cidale, L.
Formato: Artículo publishedVersion
Publicado: 2005
Materias:
Stars: early-type
Stars: mass-loss
Stars: rotation
Stars: winds, outflows
Bifurcation (mathematics)
Ionization
Mathematical models
Optical bistability
Parameter estimation
Radiation
Temperature measurement
Velocity measurement
Stars:early-type
Stars:mass-loss
Stars:rotation
Stars:winds, outflows
Astrophysics
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_00046361_v437_n3_p929_Cure
http://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_00046361_v437_n3_p929_Cure_oai
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Repositorio Digital de la Universidad de Buenos Aires (UBA) de Universidad de Buenos Aires
id I28-R145-paper_00046361_v437_n3_p929_Cure_oai
record_format dspace
spelling I28-R145-paper_00046361_v437_n3_p929_Cure_oai2020-10-19 Curé, M. Rial, D.F. Cidale, L. 2005 The effects of rapid rotation and bi-stability upon the density contrast between the equatorial and polar directions of a B[e] supergiant are re-investigated. Based on a new slow solution for different high rotational radiation-driven winds and the fact that bi-stability allows a change in the line-force parameters (α, k, and δ), the equatorial densities are about 102-104 times higher than the polar ones. These values are in qualitative agreement with the observations. © ESO 2005. Fil:Rial, D.F. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. application/pdf http://hdl.handle.net/20.500.12110/paper_00046361_v437_n3_p929_Cure info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar Astron. Astrophys. 2005;437(3):929-933 Stars: early-type Stars: mass-loss Stars: rotation Stars: winds, outflows Bifurcation (mathematics) Ionization Mathematical models Optical bistability Parameter estimation Radiation Temperature measurement Velocity measurement Stars:early-type Stars:mass-loss Stars:rotation Stars:winds, outflows Astrophysics Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds info:eu-repo/semantics/article info:ar-repo/semantics/artículo info:eu-repo/semantics/publishedVersion http://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_00046361_v437_n3_p929_Cure_oai
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-145
collection Repositorio Digital de la Universidad de Buenos Aires (UBA)
topic Stars: early-type
Stars: mass-loss
Stars: rotation
Stars: winds, outflows
Bifurcation (mathematics)
Ionization
Mathematical models
Optical bistability
Parameter estimation
Radiation
Temperature measurement
Velocity measurement
Stars:early-type
Stars:mass-loss
Stars:rotation
Stars:winds, outflows
Astrophysics
spellingShingle Stars: early-type
Stars: mass-loss
Stars: rotation
Stars: winds, outflows
Bifurcation (mathematics)
Ionization
Mathematical models
Optical bistability
Parameter estimation
Radiation
Temperature measurement
Velocity measurement
Stars:early-type
Stars:mass-loss
Stars:rotation
Stars:winds, outflows
Astrophysics
Curé, M.
Rial, D.F.
Cidale, L.
Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds
topic_facet Stars: early-type
Stars: mass-loss
Stars: rotation
Stars: winds, outflows
Bifurcation (mathematics)
Ionization
Mathematical models
Optical bistability
Parameter estimation
Radiation
Temperature measurement
Velocity measurement
Stars:early-type
Stars:mass-loss
Stars:rotation
Stars:winds, outflows
Astrophysics
description The effects of rapid rotation and bi-stability upon the density contrast between the equatorial and polar directions of a B[e] supergiant are re-investigated. Based on a new slow solution for different high rotational radiation-driven winds and the fact that bi-stability allows a change in the line-force parameters (α, k, and δ), the equatorial densities are about 102-104 times higher than the polar ones. These values are in qualitative agreement with the observations. © ESO 2005.
format Artículo
Artículo
publishedVersion
author Curé, M.
Rial, D.F.
Cidale, L.
author_facet Curé, M.
Rial, D.F.
Cidale, L.
author_sort Curé, M.
title Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds
title_short Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds
title_full Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds
title_fullStr Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds
title_full_unstemmed Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds
title_sort outflowing disk formation in b[e] supergiants due to rotation and bi-stability in radiation driven winds
publishDate 2005
url http://hdl.handle.net/20.500.12110/paper_00046361_v437_n3_p929_Cure
http://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_00046361_v437_n3_p929_Cure_oai
work_keys_str_mv AT curem outflowingdiskformationinb91e93supergiantsduetorotationandbistabilityinradiationdrivenwinds
AT rialdf outflowingdiskformationinb91e93supergiantsduetorotationandbistabilityinradiationdrivenwinds
AT cidalel outflowingdiskformationinb91e93supergiantsduetorotationandbistabilityinradiationdrivenwinds
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