Radiation-driven magnetohydrodynamic wind solutions for hot luminous stars

Solutions for the stellar winds of hot luminous stars are obtained by solving the magnetohydrodynamic (MHD) equations combined with the radiatively driven outflow formalism given by Castor, Abbott, & Klein. We consider the interaction of radiation pressure and collimated magnetic fields for a no...

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Detalles Bibliográficos
Publicado: 1996
Materias:
MHD
Stars: magnetic fields
Stars: mass loss
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v464_n2PARTI_p859_Rotstein
http://hdl.handle.net/20.500.12110/paper_0004637X_v464_n2PARTI_p859_Rotstein
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v464_n2PARTI_p859_Rotstein
record_format dspace
spelling paper:paper_0004637X_v464_n2PARTI_p859_Rotstein2023-06-08T14:28:36Z Radiation-driven magnetohydrodynamic wind solutions for hot luminous stars MHD Stars: magnetic fields Stars: mass loss Solutions for the stellar winds of hot luminous stars are obtained by solving the magnetohydrodynamic (MHD) equations combined with the radiatively driven outflow formalism given by Castor, Abbott, & Klein. We consider the interaction of radiation pressure and collimated magnetic fields for a nonrotating star. The streamline shape has been prescribed from a phenomenological point of view. In order to decouple the MHD equations, we assume all the lines contributing to the radiation pressure are optically thick. Spherically and nonspherically symmetric mass distributions are considered. In both cases, the dependence of the terminal velocity on the star luminosity and magnetic strength is discussed. It is found that the terminal flow speed is strongly affected by slight variations of both the luminosity and the mass distribution asymmetry but shows a weak correlation with the magnetic field intensity. The present formalism can be thought of as a wide generalization of the MHD solutions introduced by Low & Tsinganos. Highly collimated magnetic structures, as well as rotation, are considered in another paper. © 1996. The American Astronomical Society. All rights reserved. 1996 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v464_n2PARTI_p859_Rotstein http://hdl.handle.net/20.500.12110/paper_0004637X_v464_n2PARTI_p859_Rotstein
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic MHD
Stars: magnetic fields
Stars: mass loss
spellingShingle MHD
Stars: magnetic fields
Stars: mass loss
Radiation-driven magnetohydrodynamic wind solutions for hot luminous stars
topic_facet MHD
Stars: magnetic fields
Stars: mass loss
description Solutions for the stellar winds of hot luminous stars are obtained by solving the magnetohydrodynamic (MHD) equations combined with the radiatively driven outflow formalism given by Castor, Abbott, & Klein. We consider the interaction of radiation pressure and collimated magnetic fields for a nonrotating star. The streamline shape has been prescribed from a phenomenological point of view. In order to decouple the MHD equations, we assume all the lines contributing to the radiation pressure are optically thick. Spherically and nonspherically symmetric mass distributions are considered. In both cases, the dependence of the terminal velocity on the star luminosity and magnetic strength is discussed. It is found that the terminal flow speed is strongly affected by slight variations of both the luminosity and the mass distribution asymmetry but shows a weak correlation with the magnetic field intensity. The present formalism can be thought of as a wide generalization of the MHD solutions introduced by Low & Tsinganos. Highly collimated magnetic structures, as well as rotation, are considered in another paper. © 1996. The American Astronomical Society. All rights reserved.
title Radiation-driven magnetohydrodynamic wind solutions for hot luminous stars
title_short Radiation-driven magnetohydrodynamic wind solutions for hot luminous stars
title_full Radiation-driven magnetohydrodynamic wind solutions for hot luminous stars
title_fullStr Radiation-driven magnetohydrodynamic wind solutions for hot luminous stars
title_full_unstemmed Radiation-driven magnetohydrodynamic wind solutions for hot luminous stars
title_sort radiation-driven magnetohydrodynamic wind solutions for hot luminous stars
publishDate 1996
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v464_n2PARTI_p859_Rotstein
http://hdl.handle.net/20.500.12110/paper_0004637X_v464_n2PARTI_p859_Rotstein
_version_ 1768542766454800384

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