Magnetohydrodynamic stellar winds: A new class of solutions

This paper introduces a new class of analytic MHD solutions for steady, axisymmetric, rotating outflows interacting with poleward deflected, partially open magnetic fields. In the first paper of this series, several simplifying assumptions were necessary to deal with the problem in an analytical fas...

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Detalles Bibliográficos
Publicado: 1995
Materias:
MHD
Plasmas
Stars: mass loss
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v449_n2_p764_Rotstein
http://hdl.handle.net/20.500.12110/paper_0004637X_v449_n2_p764_Rotstein
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v449_n2_p764_Rotstein
record_format dspace
spelling paper:paper_0004637X_v449_n2_p764_Rotstein2023-06-08T14:28:33Z Magnetohydrodynamic stellar winds: A new class of solutions MHD Plasmas Stars: mass loss This paper introduces a new class of analytic MHD solutions for steady, axisymmetric, rotating outflows interacting with poleward deflected, partially open magnetic fields. In the first paper of this series, several simplifying assumptions were necessary to deal with the problem in an analytical fashion. One of the most important restrictive hypotheses is the spherical symmetry of the Mach-Alfvén surfaces. This condition is relaxed in this work, and general colatitude-dependent Alfvénic surfaces are assumed. As an example of the method, approximate solutions are found for a purely radial magnetic configuration and for initially superalfvénic outflows, by assuming a small-amplitude anisotropic component of the Mach-Alfvén function regarding the spherically symmetric part. It is shown that the general behavior of the stellar wind drastically changes. Particularly, for the sample of solutions derived here it is found that the terminal velocity of the wind does not diverge and increases with rotation. The energy distribution needed to sustain the outflow consists of a heating source located close to the photosphere, and its rate is much smaller than the blackbody power radiated by the star. The temperature profile displays the typical chromospheric structure of early-type stars once its associated set of boundary conditions is given. 1995 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v449_n2_p764_Rotstein http://hdl.handle.net/20.500.12110/paper_0004637X_v449_n2_p764_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
Plasmas
Stars: mass loss
spellingShingle MHD
Plasmas
Stars: mass loss
Magnetohydrodynamic stellar winds: A new class of solutions
topic_facet MHD
Plasmas
Stars: mass loss
description This paper introduces a new class of analytic MHD solutions for steady, axisymmetric, rotating outflows interacting with poleward deflected, partially open magnetic fields. In the first paper of this series, several simplifying assumptions were necessary to deal with the problem in an analytical fashion. One of the most important restrictive hypotheses is the spherical symmetry of the Mach-Alfvén surfaces. This condition is relaxed in this work, and general colatitude-dependent Alfvénic surfaces are assumed. As an example of the method, approximate solutions are found for a purely radial magnetic configuration and for initially superalfvénic outflows, by assuming a small-amplitude anisotropic component of the Mach-Alfvén function regarding the spherically symmetric part. It is shown that the general behavior of the stellar wind drastically changes. Particularly, for the sample of solutions derived here it is found that the terminal velocity of the wind does not diverge and increases with rotation. The energy distribution needed to sustain the outflow consists of a heating source located close to the photosphere, and its rate is much smaller than the blackbody power radiated by the star. The temperature profile displays the typical chromospheric structure of early-type stars once its associated set of boundary conditions is given.
title Magnetohydrodynamic stellar winds: A new class of solutions
title_short Magnetohydrodynamic stellar winds: A new class of solutions
title_full Magnetohydrodynamic stellar winds: A new class of solutions
title_fullStr Magnetohydrodynamic stellar winds: A new class of solutions
title_full_unstemmed Magnetohydrodynamic stellar winds: A new class of solutions
title_sort magnetohydrodynamic stellar winds: a new class of solutions
publishDate 1995
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v449_n2_p764_Rotstein
http://hdl.handle.net/20.500.12110/paper_0004637X_v449_n2_p764_Rotstein
_version_ 1768543971934470144

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