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of a polarizer in a rotatable mount calibrated in angular measure by suspending it in a beam of polarized light The exercise requires that the extinction is obtained, and the angular setting noted; after rotating the mount by 180 about the suspension axis, extinction is obtained again, and the setting noted on the mount The mid-point between the two noted angular measurements corresponds to the axis of the polarizer According to Aspnes (1970), however, small systematic errors can occur with this technique when determining the axis of prism polarizers such as the Glan Taylor air-gap calcite device It has also been noted by Serkowski (1974a) that some Polaroids are not perfect in that they may rotate the direction of vibration by as much as 0 2 To secure the reference axis of a Polaroid with respect to equatorial coordinates, Serkowski (1965) directed the telescope to the daylight cloudy sky with the telescope exactly in the meridian By placing a glass plate in a perfectly horizontal position, the telescope was adjusted in Declination so that the sky was viewed through it and the Polaroid after re ection at Brewster s angle Extinction was achieved by rotation of the Polaroid to an angular setting with uncertainty not exceeding 0 3 In the exercise to establish a set of polarization standard stars for the Hubble Space Telescope, Schmidt, Elston & Lupie (1992) measured lunar light scattered by the Earth s atmosphere in the Sun Moon Earth plane, the polarization azimuth being normal to this The direction of vibration of the polarization of light from planets or asteroids is either perpendicular or parallel to the scattering plane, according to the phase angle Calibration of the instrumental axis relative to equatorial coordinates can be obtained by observing these objects at suitable phase angles as suggested by Serkowski (1974a), following an earlier description of the process by Gehrels & Teska (1960) In the scheme devised by Dolan & Tapia (1986), a Glan Thompson prism was insertable in a slide so that its principal axis was aligned with cross-hairs of the eyepiece used to view the eld around any target star The polarimeter was then rotated on its mounting plate so that the cross-hairs were parallel to the N/S and E/W directions, this being checked by moving the telescope in these directions via the guidance controls When inserted, the polarizing prism converts any targeted star to act as a reference source with p D 100%, and with the position angle parallel to the N/S axis of equatorial coordinates For this arrangement the reference axis was determined with an uncertainty < 0 1 Another possibility might involve the use of an insertable Savart plate so that a pair of stars produces four images By rotating the plate these images may be adjusted so that they are co-linear Each of the four pencils will comprise light with p D 100%, with directions of vibration set at 45 to the line joining the images; one pair of images will carry a direction of vibration orthogonal to that of the other pair Measurement of the polarizations allows the directions of vibration to be referred to the line joining the images which in turn can be related to equatorial coordinates via the catalogued coordinates of the pair of stars Most new polarimetric studies do not undertake fundamental observational procedures as outlined above, but determine the instrumental axis by reference to.

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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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