High and intermediate-resolution spectroscopy of Be stars : An atlas of Hγ, He I 4471 and Mg II 4481 lines

Autores
Chauville, J.; Zorec, Juan; Ballereau, Dominique; Morrell, Nidia Irene; Cidale, Lydia Sonia; García, A.
Año de publicación
2001
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The definition of Be stars (Jaschek et al. 1981) as non-supergiant B stars which at least once have shown some emission in the Balmer lines implies a vast phenomenology whose characteristics, the evolution of their understanding and the questions which still remain open have been widely reviewed in the last five IAU colloquia and symposia on these stars (Slettebak 1976; Jaschek & Groth 1982; Slettebak & Snow 1987; Balona et al. 1994; Smith et al. 2000). The outstanding physical problems related to them can roughly be summarized into two groups of global questions: a) what is the nature of the central stars and when does the Be phenomenon occur during their evolutionary span?; b) what is the structure of their circumstellar envelopes (CE) and how are they produced?
Facultad de Ciencias Astronómicas y Geofísicas (FCAG)
Materia
Ciencias Astronómicas
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:10915/2084
Acceder
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oai_identifier_str oai:sedici.unlp.edu.ar:10915/2084
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling High and intermediate-resolution spectroscopy of Be stars : An atlas of Hγ, He I 4471 and Mg II 4481 linesChauville, J.Zorec, JuanBallereau, DominiqueMorrell, Nidia IreneCidale, Lydia SoniaGarcía, A.Ciencias AstronómicasAstrofísicaThe definition of Be stars (Jaschek et al. 1981) as non-supergiant B stars which at least once have shown some emission in the Balmer lines implies a vast phenomenology whose characteristics, the evolution of their understanding and the questions which still remain open have been widely reviewed in the last five IAU colloquia and symposia on these stars (Slettebak 1976; Jaschek & Groth 1982; Slettebak & Snow 1987; Balona et al. 1994; Smith et al. 2000). The outstanding physical problems related to them can roughly be summarized into two groups of global questions: a) what is the nature of the central stars and when does the Be phenomenon occur during their evolutionary span?; b) what is the structure of their circumstellar envelopes (CE) and how are they produced?Facultad de Ciencias Astronómicas y Geofísicas (FCAG)2001info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf861-882http://sedici.unlp.edu.ar/handle/10915/2084enginfo:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2001A%2526A...378..861CFULinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20011202info: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:UNLP2025-12-23T10:51:32Zoai:sedici.unlp.edu.ar:10915/2084Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-12-23 10:51:33.175SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv High and intermediate-resolution spectroscopy of Be stars : An atlas of Hγ, He I 4471 and Mg II 4481 lines
title High and intermediate-resolution spectroscopy of Be stars : An atlas of Hγ, He I 4471 and Mg II 4481 lines
spellingShingle High and intermediate-resolution spectroscopy of Be stars : An atlas of Hγ, He I 4471 and Mg II 4481 lines
Chauville, J.
Ciencias Astronómicas
Astrofísica
title_short High and intermediate-resolution spectroscopy of Be stars : An atlas of Hγ, He I 4471 and Mg II 4481 lines
title_full High and intermediate-resolution spectroscopy of Be stars : An atlas of Hγ, He I 4471 and Mg II 4481 lines
title_fullStr High and intermediate-resolution spectroscopy of Be stars : An atlas of Hγ, He I 4471 and Mg II 4481 lines
title_full_unstemmed High and intermediate-resolution spectroscopy of Be stars : An atlas of Hγ, He I 4471 and Mg II 4481 lines
title_sort High and intermediate-resolution spectroscopy of Be stars : An atlas of Hγ, He I 4471 and Mg II 4481 lines
dc.creator.none.fl_str_mv Chauville, J.
Zorec, Juan
Ballereau, Dominique
Morrell, Nidia Irene
Cidale, Lydia Sonia
García, A.
author Chauville, J.
author_facet Chauville, J.
Zorec, Juan
Ballereau, Dominique
Morrell, Nidia Irene
Cidale, Lydia Sonia
García, A.
author_role author
author2 Zorec, Juan
Ballereau, Dominique
Morrell, Nidia Irene
Cidale, Lydia Sonia
García, A.
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Astrofísica
topic Ciencias Astronómicas
Astrofísica
dc.description.none.fl_txt_mv The definition of Be stars (Jaschek et al. 1981) as non-supergiant B stars which at least once have shown some emission in the Balmer lines implies a vast phenomenology whose characteristics, the evolution of their understanding and the questions which still remain open have been widely reviewed in the last five IAU colloquia and symposia on these stars (Slettebak 1976; Jaschek & Groth 1982; Slettebak & Snow 1987; Balona et al. 1994; Smith et al. 2000). The outstanding physical problems related to them can roughly be summarized into two groups of global questions: a) what is the nature of the central stars and when does the Be phenomenon occur during their evolutionary span?; b) what is the structure of their circumstellar envelopes (CE) and how are they produced?
Facultad de Ciencias Astronómicas y Geofísicas (FCAG)
description The definition of Be stars (Jaschek et al. 1981) as non-supergiant B stars which at least once have shown some emission in the Balmer lines implies a vast phenomenology whose characteristics, the evolution of their understanding and the questions which still remain open have been widely reviewed in the last five IAU colloquia and symposia on these stars (Slettebak 1976; Jaschek & Groth 1982; Slettebak & Snow 1987; Balona et al. 1994; Smith et al. 2000). The outstanding physical problems related to them can roughly be summarized into two groups of global questions: a) what is the nature of the central stars and when does the Be phenomenon occur during their evolutionary span?; b) what is the structure of their circumstellar envelopes (CE) and how are they produced?
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/10915/2084
url http://sedici.unlp.edu.ar/handle/10915/2084
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2001A%2526A...378..861CFUL
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20011202
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
861-882
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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