S. Lepine et al., Wind inhomogeneities in Wolf-Rayet stars. IV. Using clumps to probe the wind structure in the WC8 star HD 192103, ASTRONOM J, 120(6), 2000, pp. 3201-3217
We present the most intensive, high-quality spectroscopic monitoring of opt
ical Wolf-Rayet emission lines ever obtained. The Wolf-Rayet star HD 192103
(=WR 135; subtype WC8) was observed in the 5650-5840 Angstrom regime alter
nately from both the William Herschel Telescope and the Canada-France-Hawai
i Telescope. The final data consist of a series of 197 spectra spread over
64 hr, each with a resolving power lambda/Delta lambda similar or equal to
20,000 and a signal-to-noise ratio in the continuum similar or equal to 450
per 3 pixel resolution element. We clearly and unambiguously identify stoc
hastic, structured patterns of intrinsic variability at the 1%-2% level of
the line flux in the broad C In lambda 5695 emission line. The lambda 5801/
12 doublet emission is also found to be variable at the 0.2%-0.5% level of
the line flux. We find a correlation between the variability patterns obser
ved in C III and C rv, which suggests a significant overlap in the emission
volumes of these transitions, although C Iv is known to arise somewhat clo
ser to the star. We attempt to reproduce the observed line profile variatio
n patterns using a simple phenomenological model, which assumes the wind to
be fully clumped. With a minimal set of assumptions, we are able to reprod
uce both the shape and the variability in the C III lambda 5696 emission pr
ofile. We show that the variability pattern provides constraints on the rad
ial extent of WR 135's wind where C III is produced, as well as on the loca
l wind acceleration rate. However, our simple clump model does not reproduc
e the lower variability in the C rv doublet unless we assume the C Iv emiss
ion to occur in a much larger volume than C III, implying that: significant
C Iv emission occurs farther out in the wind than C III. We suggest that w
hile some C Iv emission might occur farther out, possibly because of reioni
zation from shocks, a more likely explanation is that wind clumping signifi
cantly increases with distance from the star, leading to larger variability
levels in C III, formed farther out than most of C rv. Alternatively, opti
cal depth effects and/or local ionization gradients within clumps could con
spire to attenuate clumping effects in the C rv emission line while enhanci
ng them in the C III line.