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 change in the line-...

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Detalles Bibliográficos
Autor principal: Rial, Diego Fernando
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:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v437_n3_p929_Cure
http://hdl.handle.net/20.500.12110/paper_00046361_v437_n3_p929_Cure
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00046361_v437_n3_p929_Cure
record_format dspace
spelling paper:paper_00046361_v437_n3_p929_Cure2023-06-08T14:27:38Z Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds Rial, Diego Fernando 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 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. 2005 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v437_n3_p929_Cure http://hdl.handle.net/20.500.12110/paper_00046361_v437_n3_p929_Cure
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (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
Rial, Diego Fernando
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.
author Rial, Diego Fernando
author_facet Rial, Diego Fernando
author_sort Rial, Diego Fernando
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 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v437_n3_p929_Cure
http://hdl.handle.net/20.500.12110/paper_00046361_v437_n3_p929_Cure
work_keys_str_mv AT rialdiegofernando outflowingdiskformationinbesupergiantsduetorotationandbistabilityinradiationdrivenwinds
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