The massive Wolf-Rayet binary SMC WR7
- Autores
- Niemelä, Virpi Sinikka; Massey, P.; Testor, G.; Giménez Benítez, Sixto
- Año de publicación
- 2002
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present a study of optical spectra of the Wolf-Rayet star AzV 336a (= SMC WR7) in the Small Magellanic Cloud. Our study is based on data obtained at several Observatories between 1988 and 2001. We find SMC WR7 to be a double-lined WN+O6 spectroscopic binary with an orbital period of 19.56 d. The radial velocities of the He absorption lines of the O6 component and the strong He II emission at λ4686 Å of the WN component describe anti-phased orbital motions. However, they show a small phase shift of ∼ 1 d. We discuss possible explanations for this phase shift. The amplitude of the radial velocity variations of He II emission is twice that of the absorption lines. The binary components have fairly high minimum masses, ∼ 18 and 34 M⊙ for the WN and O6 components, respectively.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
Binaries: spectroscopic
Stars: individual: AzV 336a (=SMC WR7)
Stars: Wolf-Rayet - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/84657
Ver los metadatos del registro completo
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The massive Wolf-Rayet binary SMC WR7Niemelä, Virpi SinikkaMassey, P.Testor, G.Giménez Benítez, SixtoCiencias AstronómicasBinaries: spectroscopicStars: individual: AzV 336a (=SMC WR7)Stars: Wolf-RayetWe present a study of optical spectra of the Wolf-Rayet star AzV 336a (= SMC WR7) in the Small Magellanic Cloud. Our study is based on data obtained at several Observatories between 1988 and 2001. We find SMC WR7 to be a double-lined WN+O6 spectroscopic binary with an orbital period of 19.56 d. The radial velocities of the He absorption lines of the O6 component and the strong He II emission at λ4686 Å of the WN component describe anti-phased orbital motions. However, they show a small phase shift of ∼ 1 d. We discuss possible explanations for this phase shift. The amplitude of the radial velocity variations of He II emission is twice that of the absorption lines. The binary components have fairly high minimum masses, ∼ 18 and 34 M⊙ for the WN and O6 components, respectively.Facultad de Ciencias Astronómicas y Geofísicas2002info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf347-352http://sedici.unlp.edu.ar/handle/10915/84657enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1046/j.1365-8711.2002.05395.xinfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-03T10:48:36Zoai:sedici.unlp.edu.ar:10915/84657Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-03 10:48:36.374SEDICI (UNLP) - Universidad Nacional de La Platafalse |
| dc.title.none.fl_str_mv |
The massive Wolf-Rayet binary SMC WR7 |
| title |
The massive Wolf-Rayet binary SMC WR7 |
| spellingShingle |
The massive Wolf-Rayet binary SMC WR7 Niemelä, Virpi Sinikka Ciencias Astronómicas Binaries: spectroscopic Stars: individual: AzV 336a (=SMC WR7) Stars: Wolf-Rayet |
| title_short |
The massive Wolf-Rayet binary SMC WR7 |
| title_full |
The massive Wolf-Rayet binary SMC WR7 |
| title_fullStr |
The massive Wolf-Rayet binary SMC WR7 |
| title_full_unstemmed |
The massive Wolf-Rayet binary SMC WR7 |
| title_sort |
The massive Wolf-Rayet binary SMC WR7 |
| dc.creator.none.fl_str_mv |
Niemelä, Virpi Sinikka Massey, P. Testor, G. Giménez Benítez, Sixto |
| author |
Niemelä, Virpi Sinikka |
| author_facet |
Niemelä, Virpi Sinikka Massey, P. Testor, G. Giménez Benítez, Sixto |
| author_role |
author |
| author2 |
Massey, P. Testor, G. Giménez Benítez, Sixto |
| author2_role |
author author author |
| dc.subject.none.fl_str_mv |
Ciencias Astronómicas Binaries: spectroscopic Stars: individual: AzV 336a (=SMC WR7) Stars: Wolf-Rayet |
| topic |
Ciencias Astronómicas Binaries: spectroscopic Stars: individual: AzV 336a (=SMC WR7) Stars: Wolf-Rayet |
| dc.description.none.fl_txt_mv |
We present a study of optical spectra of the Wolf-Rayet star AzV 336a (= SMC WR7) in the Small Magellanic Cloud. Our study is based on data obtained at several Observatories between 1988 and 2001. We find SMC WR7 to be a double-lined WN+O6 spectroscopic binary with an orbital period of 19.56 d. The radial velocities of the He absorption lines of the O6 component and the strong He II emission at λ4686 Å of the WN component describe anti-phased orbital motions. However, they show a small phase shift of ∼ 1 d. We discuss possible explanations for this phase shift. The amplitude of the radial velocity variations of He II emission is twice that of the absorption lines. The binary components have fairly high minimum masses, ∼ 18 and 34 M⊙ for the WN and O6 components, respectively. Facultad de Ciencias Astronómicas y Geofísicas |
| description |
We present a study of optical spectra of the Wolf-Rayet star AzV 336a (= SMC WR7) in the Small Magellanic Cloud. Our study is based on data obtained at several Observatories between 1988 and 2001. We find SMC WR7 to be a double-lined WN+O6 spectroscopic binary with an orbital period of 19.56 d. The radial velocities of the He absorption lines of the O6 component and the strong He II emission at λ4686 Å of the WN component describe anti-phased orbital motions. However, they show a small phase shift of ∼ 1 d. We discuss possible explanations for this phase shift. The amplitude of the radial velocity variations of He II emission is twice that of the absorption lines. The binary components have fairly high minimum masses, ∼ 18 and 34 M⊙ for the WN and O6 components, respectively. |
| publishDate |
2002 |
| dc.date.none.fl_str_mv |
2002 |
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article |
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publishedVersion |
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http://sedici.unlp.edu.ar/handle/10915/84657 |
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eng |
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eng |
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info:eu-repo/semantics/altIdentifier/issn/0035-8711 info:eu-repo/semantics/altIdentifier/doi/10.1046/j.1365-8711.2002.05395.x |
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http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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