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
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/2087
Ver los metadatos del registro completo
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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:UNLP2025-09-29T10:48:37Zoai: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:13292025-09-29 10:48:39.097SEDICI (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 |
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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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1844615739255816192 |
score |
13.070432 |