Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...683..449b&link_type=abstract
The Astrophysical Journal, Volume 683, Issue 1, pp. 449-465.
Astronomy and Astrophysics
Astronomy
Line: Profiles, Stars: Individual (Br 22), Stars: Individual (Br 32), Stars: Wolf-Rayet, Techniques: Spectroscopic
Scientific paper
Using the Far Ultraviolet Spectroscopic Explorer satellite, we obtained series of spectra for two of the three known WC + O binaries in the LMC, Br 22, and Br 32 (HD 36521). Compared to Br 22, we detect a higher ratio of C IV to He II lines in Br 32, which could indicate a more advanced evolutionary stage for the latter. The orbit of the O star in Br 32 has been determined from its P V absorption lines. We find that continuum fluxes in both systems are substantially diluted by a third-light source. The maximum extension of the black absorption troughs in P Cygni profiles provides the terminal velocities of the WC winds: 3775+/-125 km s-1 for Br 22 and 4400+/-150 km s-1 for Br 32. From the phase-dependent displacements of the blue absorption edges of prominent emission lines we estimate the half-opening angles of the wind-wind collision zones and their Coriolis deflections. In both binaries we fitted, via iterative procedure, the phase-dependent changes in the O VI λ1032-1037 and C III λ1175 profiles as a function of the wind, stellar, and orbital parameters. This allowed us to isolate the excess emission produced in the wind-wind collision zone and reproduce profile changes caused by atmospheric eclipses. A strong extra emission component is observed in Br 22 (P=14.9 days), while it is negligible in Br 32 (P=1.9 days).
Based on observations made with the NASA-CNES-CSA Far Ultraviolet Spectroscopic Explorer (FUSE). FUSE is operated for NASA by The Johns Hopkins University under NASA contract NAS5-32985.
Boisvert Philippe
Marchenko Sergey V.
Moffat Anthony F. J.
St-Louis Nicole
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