A SPECTROPOLARIMETRIC SURVEY OF NORTHERN-HEMISPHERE WOLF-RAYET STARS

We present a homogeneous, high signal-to-noise spectropolarimetric sun ?ey of 16 northern hemisphere Wolf-Rayet (WR) stars. A reduction in po larization at emission-line wavelengths - the 'line effect' - is ident ified in four stars: WRs 134, 137, 139, and 141. The magnitude of the effect in WR 139 (V444 Cyg) is variable, while WR 136, previously repo rted to show the line effect, does not show it in our data. Assuming t he line effect generally to arise from axisymmetric distortions of ste llar winds, we show that a model in which all WRs have the same intrin sic (equator-on) polarization, with the observed variations solely a r esult of inclination effects, is inconsistent with the observations. A model in which the intrinsic polarizations are uniformly distributed is more plausible, but best-fitting results are obtained if the distri bution of polarizations is biased towards small values. with only simi lar to 20 per cent of stars having intrinsic polarizations greater tha n similar to 0.3 per cent. Radiative transfer calculations indicate th at the observed continuum polarizations can be matched by models with equator:pole density ratios of 2-3. The model spectra have electron-sc attering wings that are significantly stronger than observed tin both intensity and polarized flux), confirming that the winds of stars show ing intrinsic polarization must be clumped on small scales as well as being distorted on large scales. We combine the results of our survey with observations from the literature to give a sample of 29 stars whi ch have both accurate spectropolarimetric observations and physical pa rameters derived from standard-model analyses. We find that the line-e ffect stars are clustered at high (M) over dot. L in the luminosity-ma ss-loss rate plane (although they are unexceptional in the terminal ve locity-subtype and the surface-mass-flux-temperature planes). The mass -loss rates derived from radio-continuum observations for these stars are in good accord with the results of optical emission-line analyses, suggesting that ii) the wind structure of line-effect stars has a den sity contrast which is effectively constant with radius, and (ii) the high (M) over dot values may be artefacts of large-scale wind structur e. Assuming that observed spectroscopic and photometric variability of the line-effect stars is related to the WR rotation period, we comput e equatorial rotation velocities. These velocities correspond to simil ar to 10 per cent of the core breakup rates, and may be large enough t o produce significant wind-compression effects according to the models of Ignace, Cassinelli & Bjorkman.