To be published in:
Astronomy and Astrophysics
The strange case of the massive binary HD149404+
E. Gosset1,** and
1 Institut d'Astrophysique et de Géophysique - Université de Liège, Avenue de Cointe 5, 4000 Liège, Belgium
2 Observatoire de Genève, CH-1290 Sauverny, Switzerland
* Postdoctoral Researcher FNRS, Belgium
** Research Associate FNRS, Belgium
+ Based on observations collected at the European Southern Observatory (La Silla, Chile) and at the Cerro Tololo Inter-American Observatory (CTIO)
We report the analysis of an extensive set of high-resolution spectroscopic
observations of the massive binary system HD149404. We compare different
techniques to measure the radial velocities of the heavily blended
absorption lines and we derive a new orbital solution. The absorption lines
display strong variability that slightly affects the orbital solution and
the determination of the spectral types of the components of the binary.
We find that the primary is probably of spectral type O7.5 I(f), while the
secondary is most likely an ON9.7 I supergiant.
stars: early-type -- binaries: spectroscopic -- stars: individual: HD149404
The secondary seems to be the most evolved component of the system and its
current evolutionary status could best be explained if the system has
undergone a Roche lobe overflow episode during the past. The secondary could
actually still be rather close to filling its critical volume and this could
lead to an enhanced mass loss of the secondary.
The spectrum of HD149404 displays many emission lines some of which show
phase-locked line profile variations. In particular, the
H line displays a double-peaked morphology
at orbital phases near conjunction. We investigate the radial velocity
behaviour of the emission lines and we find that some of them must be formed
in an interaction region. We propose a simple model where some of the
optical emission lines arise in a heavily bended shock region.