Diagnosis of stellar winds and temperature structures in Be stars through the analysis of Mg II lines

Autores
Cidale, Lydia Sonia
Año de publicación
1998
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We compute non-LTE Mg II line profiles for Be stars by considering 12 energy-level atoms and supposing that the circumstellar medium can be described by an expanding, spherically symmetric flow in which we assume the presence of a chromosphere. The line radiative transfer equation was solved rigorously in spherical coordinates and in the comoving frame. The Mg II line profiles predicted by this model coincide with those observed in some Be stars. The calculation was performed for a range of effective temperatures representative of the B spectral type. We have also analyzed the influence on the line profiles of different temperature and velocity distributions in the circumstellar material. The line spectrum variability of a Be star is interpreted as the result of a variable outward mass flux.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
estrellas
circumstellar matter; radiative transfer; emission line; Be stars; mass loss
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:10915/2087
Acceder
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oai_identifier_str oai:sedici.unlp.edu.ar:10915/2087
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Diagnosis of stellar winds and temperature structures in Be stars through the analysis of Mg II linesCidale, Lydia SoniaCiencias Astronómicasestrellascircumstellar matter; radiative transfer; emission line; Be stars; mass lossastrofísicaWe compute non-LTE Mg II line profiles for Be stars by considering 12 energy-level atoms and supposing that the circumstellar medium can be described by an expanding, spherically symmetric flow in which we assume the presence of a chromosphere. The line radiative transfer equation was solved rigorously in spherical coordinates and in the comoving frame. The Mg II line profiles predicted by this model coincide with those observed in some Be stars. The calculation was performed for a range of effective temperatures representative of the B spectral type. We have also analyzed the influence on the line profiles of different temperature and velocity distributions in the circumstellar material. The line spectrum variability of a Be star is interpreted as the result of a variable outward mass flux.Facultad de Ciencias Astronómicas y Geofísicas1998info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf824-832http://sedici.unlp.edu.ar/handle/10915/2087enginfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1086/305918info:eu-repo/semantics/altIdentifier/issn/0004-637Xinfo: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:UNLP2025-10-22T16:30:18Zoai:sedici.unlp.edu.ar:10915/2087Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-10-22 16:30:18.954SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Diagnosis of stellar winds and temperature structures in Be stars through the analysis of Mg II lines
title Diagnosis of stellar winds and temperature structures in Be stars through the analysis of Mg II lines
spellingShingle Diagnosis of stellar winds and temperature structures in Be stars through the analysis of Mg II lines
Cidale, Lydia Sonia
Ciencias Astronómicas
estrellas
circumstellar matter; radiative transfer; emission line; Be stars; mass loss
astrofísica
title_short Diagnosis of stellar winds and temperature structures in Be stars through the analysis of Mg II lines
title_full Diagnosis of stellar winds and temperature structures in Be stars through the analysis of Mg II lines
title_fullStr Diagnosis of stellar winds and temperature structures in Be stars through the analysis of Mg II lines
title_full_unstemmed Diagnosis of stellar winds and temperature structures in Be stars through the analysis of Mg II lines
title_sort Diagnosis of stellar winds and temperature structures in Be stars through the analysis of Mg II lines
dc.creator.none.fl_str_mv Cidale, Lydia Sonia
author Cidale, Lydia Sonia
author_facet Cidale, Lydia Sonia
author_role author
dc.subject.none.fl_str_mv Ciencias Astronómicas
estrellas
circumstellar matter; radiative transfer; emission line; Be stars; mass loss
astrofísica
topic Ciencias Astronómicas
estrellas
circumstellar matter; radiative transfer; emission line; Be stars; mass loss
astrofísica
dc.description.none.fl_txt_mv We compute non-LTE Mg II line profiles for Be stars by considering 12 energy-level atoms and supposing that the circumstellar medium can be described by an expanding, spherically symmetric flow in which we assume the presence of a chromosphere. The line radiative transfer equation was solved rigorously in spherical coordinates and in the comoving frame. The Mg II line profiles predicted by this model coincide with those observed in some Be stars. The calculation was performed for a range of effective temperatures representative of the B spectral type. We have also analyzed the influence on the line profiles of different temperature and velocity distributions in the circumstellar material. The line spectrum variability of a Be star is interpreted as the result of a variable outward mass flux.
Facultad de Ciencias Astronómicas y Geofísicas
description We compute non-LTE Mg II line profiles for Be stars by considering 12 energy-level atoms and supposing that the circumstellar medium can be described by an expanding, spherically symmetric flow in which we assume the presence of a chromosphere. The line radiative transfer equation was solved rigorously in spherical coordinates and in the comoving frame. The Mg II line profiles predicted by this model coincide with those observed in some Be stars. The calculation was performed for a range of effective temperatures representative of the B spectral type. We have also analyzed the influence on the line profiles of different temperature and velocity distributions in the circumstellar material. The line spectrum variability of a Be star is interpreted as the result of a variable outward mass flux.
publishDate 1998
dc.date.none.fl_str_mv 1998
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/10915/2087
url http://sedici.unlp.edu.ar/handle/10915/2087
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1086/305918
info:eu-repo/semantics/altIdentifier/issn/0004-637X
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
824-832
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 12.982451

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