Estrellas Be: formación de líneas de Mg II en un viento estelar

We have worked out the equations of conservation of mass, momentum and energy for the case of steady outflows in a rotating magnetic field, introducing a polytropic-type relation between pressure and density, with a variable index. We have determined sets of parameters that bring up the critical poi...

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Detalles Bibliográficos
Autor principal: Cidale, Lydia Sonia
Formato: Articulo Comunicacion
Lenguaje:Español
Publicado: 1992
Materias:
Astronomía
Galaxia
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/143631
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-143631
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Español
topic Astronomía
Galaxia
spellingShingle Astronomía
Galaxia
Cidale, Lydia Sonia
Estrellas Be: formación de líneas de Mg II en un viento estelar
topic_facet Astronomía
Galaxia
description We have worked out the equations of conservation of mass, momentum and energy for the case of steady outflows in a rotating magnetic field, introducing a polytropic-type relation between pressure and density, with a variable index. We have determined sets of parameters that bring up the critical points that are needed to select a unique solution for the wind and finally, we have chosen those sets that can reproduce better the conditions observed in Be stars. Each solution depends on the choice of six non-dimensional parameters which are related to the fluxes of energy at the base of the wind and at infinity, to the gravitational field, to the effective temperature of the star, to rotation and to the magnetic field. The corotation induced by the magnetic field increases the centrifugal force and accelerates the wind. The choice of a particular functional form for the polytropic index allows the formation of a heating-accelerating region where the temperature increases with expansion and where larger temperatures and larger expansion values are obtained for strongly magnetized flows. Outside this region, temperature and rotation decay and the magnetic field yields two solutions of different asymptotic behaviour; in one solution the velocity accelerates and in the other the velocity decelerates, until they reach constant values.
format Articulo
Comunicacion
author Cidale, Lydia Sonia
author_facet Cidale, Lydia Sonia
author_sort Cidale, Lydia Sonia
title Estrellas Be: formación de líneas de Mg II en un viento estelar
title_short Estrellas Be: formación de líneas de Mg II en un viento estelar
title_full Estrellas Be: formación de líneas de Mg II en un viento estelar
title_fullStr Estrellas Be: formación de líneas de Mg II en un viento estelar
title_full_unstemmed Estrellas Be: formación de líneas de Mg II en un viento estelar
title_sort estrellas be: formación de líneas de mg ii en un viento estelar
publishDate 1992
url http://sedici.unlp.edu.ar/handle/10915/143631
work_keys_str_mv AT cidalelydiasonia estrellasbeformaciondelineasdemgiienunvientoestelar
bdutipo_str Repositorios
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