Open AccessSpectroscopic study of the long‐period dust‐producing WC7pd+O9 binary HD 192641
Author(s) -
Lefèvre L.,
Marchenko S. V.,
Lépine S.,
Moffat A. F. J.,
Acker A.,
Harries T. J.,
Annuk K.,
Bohlender D. A.,
Demers H.,
Grosdidier Y.,
Hill G. M.,
Morrison N. D.,
Knauth D. C.,
Skalkowski G.,
Viti S.
Publication year - 2005
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2005.09017.x
Subject(s) - physics , astrophysics , wolf–rayet star , ionization , emission spectrum , spectral line , amplitude , astronomy , stars , optics , ion , quantum mechanics
We present the results of an optical spectroscopic study of the massive Wolf–Rayet (WR) binary HD 192641 = WR 137 . These 1986–2000 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 4766 ± 66 d (13.05 ± 0.18 yr) . The resulting masses, adopting i = 67 ° , are M O = 20 ± 2 M ⊙ for the O component and M WR = 4.4 ± 1.5 M ⊙ for the WR component. These appear, respectively, approximately normal and on the low side for the given spectral types. Analysis of the intense multisite spectroscopic monitoring in 1999 shows that the C iii λ5696 and C iv λλ5802/12 lines have the highest intrinsic variability levels. The periodogram analysis yields a small‐amplitude modulation in the absorption troughs of the C iv λλ5802/12 and He i λ5876 lines with a period of 0.83 d, which could be related either to pulsations or large‐scale rotating structures as seen in the WN4 star EZ Canis Majoris (WR 6). Wavelet analysis of the strong emission lines of C iii λ5696 and C iv λλ5802/12 enabled us to isolate and follow for several hours small structures (emission subpeaks) 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 variability in emission lines with different ionization potentials, i.e. in lines formed at different distances from the WR stellar core. Adopting a β wind‐velocity law, from the motion of individual subpeaks we find β∼ 5 , which is significantly larger than the canonical value β≃ 1 found in O star winds.