The massive Wolf-Rayet binary SMC WR7
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...
| Autores: | , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2002 |
| País: | Argentina |
| Institución: | Universidad Nacional de La Plata |
| Repositorio: | SEDICI (UNLP) |
| Idioma: | inglés |
| OAI Identifier: | oai:sedici.unlp.edu.ar:10915/84657 |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/84657 |
| Access Level: | acceso abierto |
| Palabra clave: | Ciencias Astronómicas Binaries: spectroscopic Stars: individual: AzV 336a (=SMC WR7) Stars: Wolf-Rayet |
| Sumario: | 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. |
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