Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jrasc..99t.133b&link_type=abstract
Journal of the Royal Astronomical Society of Canada, Vol. 99, No. 4, p.133
Astronomy and Astrophysics
Astronomy
Scientific paper
O stars are the most massive of the main-sequence stars. Wolf-Rayet (WR) stars are evolved O stars that have lost most or all of their hydrogen. Both emit stellar winds with very high terminal velocity and very high density. The mass loss for these stars is then also very high, and that affects profoundly their evolution. Such strong winds also have impacts on the local interstellar medium by pushing it and by increasing its metallicity. For all these reasons, it is of the greatest interest to better know the properties of these winds. One of the best ways to do it is to study the wind-wind collision in a O+WR binary system. Such a collision leads to the formation of a cone-shaped shock surface around the star having the wind with the lowest momentum. This cone spins with the orbital motion, which induces variations in the binary spectrum with phase. These variations allow deducing a lot of information about the geometry of the shock cone and about the winds of both stars. My project is on two WR+O binaries in the Large Magellanic Cloud (LMC): Br22 and Br32. These two systems have almost identical spectral types (WC4+O5-6 III-V), but have periods of respectively 14.9 and 1.9 days. This great similitude makes them very interesting to study in parallel. Also, both systems have been intensively studied in the optical spectrum recently (Bartzakos 2001). My work is to complement this latter work by studying the far ultraviolet portion of the spectra, obtained at different phases with the Far Ultraviolet Spectroscopic Explorer (FUSE), a satellite spectroscopic telescope. The strongest lines in this portion is Ovi_1032-1037 (Ovi is only observable with FUSE) and Ciii_1175. I fitted these lines with a program made by Sergey Marchenko. This code accounts for the orbital geometry of the stars and the cone, the atmospheric eclipses, and the extra emission produced by the shock region. With that, I have been able to put constraints on many parameters of the stellar winds in Br22 and Br32.
Boisvert Philippe
Marchenko Sergey V.
Moffat Anthony F. J.
St-Louis Nicole
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