The very massive X-ray bright binary system Wack 2134 (= WR 21a)
From the radial velocities of the N IV λ4058 and He II λ4686 emission lines, and the N v λ4604-20 absorption lines, determined in digital spectra, we report the discovery that the X-ray bright emission line star Wack 2134 (= WR 21a) is a spectroscopic binary system with an orbital period of 31.673 ±...
| Autores principales: | , , , , , , , |
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| Formato: | Articulo |
| Lenguaje: | Inglés |
| Publicado: |
2008
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| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/84153 |
| Aporte de: |
| id |
I19-R120-10915-84153 |
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| record_format |
dspace |
| institution |
Universidad Nacional de La Plata |
| institution_str |
I-19 |
| repository_str |
R-120 |
| collection |
SEDICI (UNLP) |
| language |
Inglés |
| topic |
Ciencias Astronómicas Binaries: spectroscopic Stars: individual: Wack 2134 Stars: individual: WR 21a Stars: Wolf-Rayet |
| spellingShingle |
Ciencias Astronómicas Binaries: spectroscopic Stars: individual: Wack 2134 Stars: individual: WR 21a Stars: Wolf-Rayet Niemelä, Virpi Sinikka Gamen, Roberto Barbá, Rodolfo Héctor Fernández Lajús, Eduardo Benaglia, Paula Solivella, Gladys Rebeca Reig, P. Coe, M. J. The very massive X-ray bright binary system Wack 2134 (= WR 21a) |
| topic_facet |
Ciencias Astronómicas Binaries: spectroscopic Stars: individual: Wack 2134 Stars: individual: WR 21a Stars: Wolf-Rayet |
| description |
From the radial velocities of the N IV λ4058 and He II λ4686 emission lines, and the N v λ4604-20 absorption lines, determined in digital spectra, we report the discovery that the X-ray bright emission line star Wack 2134 (= WR 21a) is a spectroscopic binary system with an orbital period of 31.673 ± 0.002 d. With this period, the N IV and He II emission and N v absorption lines, which originate in the atmosphere of the primary component, define a rather eccentric binary orbit (e = 0.64 ± 0.03). The radial velocity variations of the N v absorptions have a lower amplitude than those of the He II emission. Such a behaviour of the emission line radial velocities could be due to distortions produced by a superimposed absorption component from the companion. High-resolution echelle spectra observed during the quadrature phases of the binary show H and He II absorptions of both components with a radial velocity difference of about 541 km s<SUP>-1</SUP>. From this difference, we infer quite high values of the minimum masses, of about 87 and 53 M⊙ for the primary and secondary components, respectively, if the radial velocity variations of the He II emission represent the true orbit of the primary. No He i absorption lines are observed in our spectra. Thus, the secondary component in the Wack 2134 binary system appears to be an early O-type star. From the presence of H, He II and N v absorptions, and N IV and C IV emissions, in the spectrum of the primary component, it most clearly resembles those of Of/WNLha-type stars. |
| format |
Articulo Articulo |
| author |
Niemelä, Virpi Sinikka Gamen, Roberto Barbá, Rodolfo Héctor Fernández Lajús, Eduardo Benaglia, Paula Solivella, Gladys Rebeca Reig, P. Coe, M. J. |
| author_facet |
Niemelä, Virpi Sinikka Gamen, Roberto Barbá, Rodolfo Héctor Fernández Lajús, Eduardo Benaglia, Paula Solivella, Gladys Rebeca Reig, P. Coe, M. J. |
| author_sort |
Niemelä, Virpi Sinikka |
| title |
The very massive X-ray bright binary system Wack 2134 (= WR 21a) |
| title_short |
The very massive X-ray bright binary system Wack 2134 (= WR 21a) |
| title_full |
The very massive X-ray bright binary system Wack 2134 (= WR 21a) |
| title_fullStr |
The very massive X-ray bright binary system Wack 2134 (= WR 21a) |
| title_full_unstemmed |
The very massive X-ray bright binary system Wack 2134 (= WR 21a) |
| title_sort |
very massive x-ray bright binary system wack 2134 (= wr 21a) |
| publishDate |
2008 |
| url |
http://sedici.unlp.edu.ar/handle/10915/84153 |
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