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The issue of whether O-type stars which, from their spectra, are known to possess variable wind structures has been taken up by Clarke, McDavid, Smith, et al (2002) For Per and Cep, analysis of a series of measurements made on single nights with individual uncertainties of p 00002, with nightly means carrying uncertainties of p 000007, suggested night-to-night variations with p 00002 It was suggested that such low-level uctuations might be engendered by structured instrumental polarization in the stellar diffraction pattern, and instrumental depolarization effects that will induce polarimetric noise according to inconsistent target acquisition and/or the action of variable seeing conditions Reassessment of the older data for Cep from Hayes (1978) also suggested that his claims for the detection of variability of this star suffer from the same problems Whether or not such supergiant stars do exhibit polarization variability requires further observational work, with careful attention being paid to the stability of repeated measurements With the advent of CCD spectropolarimetry, Harries & Howarth (1996) have investigated the H emission line of Pup (O4 I(n)f) Although data from their instrument suffered from polarizance fringes, a correction procedure was applied with the results showing that there is a polarization signature across the H emission of this star The feature is attributed to an equatorial density enhancement of the wind, their numerical model suggesting a factor of 13 for the equator-to-pole density ratio Harries (2000) has applied Monte Carlo principles to set up stellar wind radiativetransfer codes Effects of co-rotating spiral density enhancements and also effects of clumpiness within the wind were investigated Although the test runs reproduce the observed spectrometric variability of OB supergiants, the suggested polarimetric variability of these models is too weak to explain the observed behaviour of these stars A predicted spectral line polarization was noted resulting from line absorption of continuum photons in a rotating wind, the ffect having a strong resemblance to the H polarimetric signal recorded by Harries & Howarth (1996) for Pup It is suggested that the recorded behaviour stems from this effect, rather than by line dilution of a continuum polarization It is of interest to note that an attempt was made by Hanbury Brown, David & Allan (1974) to measure the diameter of the supergiant Ori with orthogonal polarizations, using the Narrabri stellar intensity interferometer, in an attempt to detect any geometric distortion of the star s corona No signi cant changes of correlation were detected for the two polarizations, with no changes in the apparent diameter of the star An assessment of the possibility of success with this kind of observational technique was undertaken by Sams & Johnston (1974) using stellar models to predict the polarization It was concluded that the sensitivity would require improvements of 20 times, or more, to detect photospheric polarization in early-type stars In view of the success of other interferometric observations at H in respect of Be stars with disc structures, as described in Section 133, neglect of application of the intensity interferometer at this wavelength would seem to have missed out on making a substantial contribution here.



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the single-scattering plus attenuation prediction For these reasons, the combined effects of multiple scattering, plus absorptive opacity, provides much larger polarization discontinuities at the Balmer jump than previous predictions For geometrically thick equatorial disc-like geometries, a position angle ip of 90 can occur shortward of the Balmer jump as the large hydrogen opacity absorbs the multiply scattered photons in the disc, the polarization dominated by singly scattered photons from the polar regions producing negative values of Q Using a Monte Carlo radiative transfer code in respect of spectropolarimetric data, Wood, Bjorkman & Bjorkman (1997) investigated possible geometries for Tau It turned out that the observations could be mimicked by either a geometrically thin disc, with a half-opening angle of 2 5, or a thick disc with a half-opening angle of 56 Key to determining which option should be preferred is the prediction for the thin disc model to produce a polarization ip at 12 m, so that it is orthogonal relative to what is recorded in the visible spectrum As for interpretations and modelling of p ( ) and the intrinsic polarizations associated with the emission lines themselves, McLean (1979) discussed the issues with physical insight The paper demonstrates that all axisymmetric, quasi-optically thin Be star envelopes have approximately the same form of p ( ) in the continuum and that the behaviour is controlled by the average properties of the envelope The size of the oscillation of the position angle across the emission lines, as well as depending on the optical depths of the envelope, is shown to be proportional to cos i A numerical model for the behaviour of Cas was presented by Poeckert & Marlborough (1978a) by assuming a density distribution in a rotating, expanding envelope, with the hydrogen level populations determined appropriately at points through the envelope The Balmer line intensities and polarimetric pro les were then determined by integrating the equation of radiative transfer along the lines of sight, and so including stellar disc occultation effects in the process The exercise was successful in predicting the observed behaviour across the H line An investigation of the physical factors that control the behaviour of p ( ) and ( ) across emission line pro les has been made by Wood, Brown & Fox (1993) based on Thomson scattering in an optically thin circumstellar cloud which is subject to bulk motions in the form of a rotating and/or expanding disc The value of p is asymmetric about the line centre and stronger in the red wing unless there is no disc expansion Changes in across the line occur through the symmetry breaking effects of stellar occultation of the scattering material, and the combination of rotation and expansion of the disc A symmetric p pro le indicates envelope rotation, while pro les which show stronger p in the red wing indicate expansion of a scattering region The ratio of p in the red and blue wings should lead to information on the ratios of expansion to rotation velocities In a later paper, Wood & Brown (1994a) developed the model by considering the star to act as a monochromatic source for scattering by a rotating and expanding isc, the assumption being reasonably realistic, the line broadening being dominated by the scattering rather than in its origins By assuming certain parametric forms for the disc velocity and density distributions, analytic expressions were obtained for the wavelength dependence of the scattered pro les in terms of the veloc-.

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