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

Autores
Curé, Michel; Cidale, Lydia Sonia
Año de publicación
2001
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
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.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
Geofísica, astronomía y astrofísica
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-nd/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/2085
Acceder
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oai_identifier_str oai:sedici.unlp.edu.ar:10915/2085
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar windsCuré, MichelCidale, Lydia SoniaCiencias AstronómicasGeofísica, astronomía y astrofísicaLine 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.Facultad de Ciencias Astronómicas y Geofísicas2001info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf415-418http://sedici.unlp.edu.ar/handle/10915/2085enginfo:eu-repo/semantics/altIdentifier/url/http://articles.adsabs.harvard.edu//full/2001ASPC..248..415C/0000415.000.htmlinfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-nd/4.0/Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-03T10:21:37Zoai:sedici.unlp.edu.ar:10915/2085Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-03 10:21:38.182SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds
title Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds
spellingShingle Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds
Curé, Michel
Ciencias Astronómicas
Geofísica, astronomía y astrofísica
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
dc.creator.none.fl_str_mv Curé, Michel
Cidale, Lydia Sonia
author Curé, Michel
author_facet Curé, Michel
Cidale, Lydia Sonia
author_role author
author2 Cidale, Lydia Sonia
author2_role author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Geofísica, astronomía y astrofísica
topic Ciencias Astronómicas
Geofísica, astronomía y astrofísica
dc.description.none.fl_txt_mv 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.
Facultad de Ciencias Astronómicas y Geofísicas
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.
publishDate 2001
dc.date.none.fl_str_mv 2001
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/2085
url http://sedici.unlp.edu.ar/handle/10915/2085
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://articles.adsabs.harvard.edu//full/2001ASPC..248..415C/0000415.000.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-nd/4.0/
Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-nd/4.0/
Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)
dc.format.none.fl_str_mv application/pdf
415-418
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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score 13.13397

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