Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds

Line driven wind theory has been improved including non-spherical expansion in order to study its influence upon disk formation in early-type stars. Assuming that magnetic field controls the flow geometry, the plasma must flow downstream through open magnetic field lines. It is found that in the pol...

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Detalles Bibliográficos
Autores principales: Curé, Michel, Cidale, Lydia Sonia
Formato: Articulo
Lenguaje:Inglés
Publicado: 2001
Materias:
Ciencias Astronómicas
Geofísica, astronomía y astrofísica
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/2085
http://articles.adsabs.harvard.edu//full/2001ASPC..248..415C/0000415.000.html
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-2085
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
Geofísica, astronomía y astrofísica
spellingShingle Ciencias Astronómicas
Geofísica, astronomía y astrofísica
Curé, Michel
Cidale, Lydia Sonia
Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds
topic_facet Ciencias Astronómicas
Geofísica, astronomía y astrofísica
description Line driven wind theory has been improved including non-spherical expansion in order to study its influence upon disk formation in early-type stars. Assuming that magnetic field controls the flow geometry, the plasma must flow downstream through open magnetic field lines. It is found that in the polar direction rapid flow tube divergence almost does not modify the location of the critical (singular) point and the calculated terminal velocity is incremented about 400 km/sec. On the other band in the equatorial direction, for a fast rotation case, the location of the critical point is unchanged and the terminal velocity shows slightly variations of about 50 km/sec. This conclusion is the polar direction is contrary to previous results, where the finite disk correction has not been taken into account. These results suggest, that open magnetic field lines do not influence disk formation in Be-stars.
format Articulo
Articulo
author Curé, Michel
Cidale, Lydia Sonia
author_facet Curé, Michel
Cidale, Lydia Sonia
author_sort Curé, Michel
title Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds
title_short Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds
title_full Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds
title_fullStr Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds
title_full_unstemmed Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds
title_sort influence of magnetic in be-stars disk formation due to rotation in line driven in stellar winds
publishDate 2001
url http://sedici.unlp.edu.ar/handle/10915/2085
http://articles.adsabs.harvard.edu//full/2001ASPC..248..415C/0000415.000.html
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AT cidalelydiasonia influenceofmagneticinbestarsdiskformationduetorotationinlinedriveninstellarwinds
bdutipo_str Repositorios
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