Spectroscopic study of the long-period dust-producing WC7pd+O9 binary HD192641

Abstract

We present the results of an optical spectroscopic study of the massive Wolf-Rayet binary WR137. These data cover the dust-formation maximum in 1997. Combining all available measurements of radial velocities, we derive, for the first time, a spectroscopic orbit with period 13.05 +/- 0.18 years. The resulting masses, adopting i=67degrees, are M(O)= 20 +/- 2 Mo and M(WR)= 4.4+/- 1.5 Mo. These appear, respectively, around normal and on the low side for the given spectral types. Analysis of the intense multi-site spectroscopic monitoring in 1999 shows that the CIII5696 and CIV5802/12 lines have the highest intrinsic variability levels. The periodogram analysis yields a small-amplitude modulation in the absorption troughs of the CIV5802/12 and HeI5876 lines with a period of 0.83 days, which could be related either to pulsations or large-scale rotating structures as seen in the WN4 star EZ Canis Majoris (WR6).Wavelet analysis of the strong emission lines of CIII5696 and CIV5802/12 enabled us to isolate and follow for several hours small structures associated with density enhancements within the wind of the Wolf-Rayet star. Cross-correlating the variability patterns seen in different lines, we find a weak but significant correlation between the varability in emission lines with different ionization potential, i.e. in lines formed at different distances from the WR stellar core. Adopting a beta wind-velocity law, from the motion of individual subpeaks we find beta around 5, which is significantly larger than the canonical value of 1 usually found in O-star winds.

arXiv comment14 pages, 12 figures

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