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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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expected net polarization, while at high inclination, the polarization is reduced by occultation Their analysis was also applied to the variation of polarization from binary systems in which the scattering material consists of a rotating onedimensional plume etween the stars, superposed on an axisymmetric disc They showed that the inclination of the system and the radial structure of the plume can be deduced for suf ciently high inclinations (i > 60 ) The extent to which the method can be generalized to an arbitrarily distributed two-dimensional scattering region was considered via Fourier analysis It was found that the inclination of the system is largely insensitive to the density distribution when the distribution function is of a simple power-law form The question was also raised that for some stars, the polar mass loss will have a greater ionization fraction than the equatorial region, such that the pole might be the dominant source for free electrons In the third paper of this series, Fox (1991) considered the effects of occultation and nite sized-source depolarization, concluding that the net polarization has a complicated inclination dependence, and that the simple result of it being p / sin2 i, obtained by Brown & McLean (1977), does not hold For Be stars with high intrinsic polarizations, the circumstellar envelope must be concentrated either towards equatorial or polar regions, and that a substantial optical depth is required with > 005 The possible variability of the observed polarization from an obliquely rotating envelope has been investigated by Fox (1992), such a scenario having been mooted by others as being an alternative interpretation to diagnoses involving binary motion, but with lack of spectroscopic evidence to add weight to such duplicity The results of the exercise were not too sanguine as it was evident that effects due to rotation about a body axis and binary orbital motion are indistinguishable It was also found that the physical geometry of the obliquely rotating envelope could not be inferred When the light source is considered to have nite extent, discrimination between envelope geometries emerges to some degree as a result of the occultation of parts of the envelope by the extended source Further modelling by Fox (1993a) has emphasized the effect that an extended light source has on the resulting polarization by scattering in circumstellar envelopes If the underlying star is non-spherical, as a result of its large rotational velocity say, its photosphere will also generate a net polarization, adding to that which is produced by scattering within the extended atmosphere This situation has been modelled by Fox (1993a) who found that, in general, the predicted polarization was a factor of 2 3 times larger than what is observed for Be star systems It was also noted that the theoretical models for Be star envelopes had not yet reached a level of sophistication to estimate by polarimetry the number density of free electrons throughout the circumstellar envelope The origin of stellar winds in Be stars may be in uenced by magnetic elds and Fox (1993b) has considered this additional parameter in polarimetric models From his analysis, the range of observed values of p can be explained if the stars possess small magnetic elds of B0 < 100 G Observed increases in p during the onset of a shell phase is indicative of an increased magnetic eld.

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