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Figure 151) Clarke & Fullerton (1996) also monitored polarimetric variations between p 000001 and 00001 in the global light during a time when the Sun was close to sunspot maximum, with the effects of the passage of a large sunspot group moving across the disc being detectable Coyne (1974) has described a preliminary investigation of faint stars in the Pleiades, these being young solar-types His work suggested a number of them exhibited intrinsic polarization by the fact that the value of p is largest in the ultraviolet At the time, the discussion was related to elementary structure of the nebulosity within the Pleiades It may be possible that some polarization may be engendered by are-like and spot activity which many of the early solar-type stars in the Pleiades are known to exhibit Ellias II & Dorren (1990) recorded polarimetric variability for the young 70 Myr solar-type star HD 129333, probably a member of the Pleiades moving group Broadband measurements indicated that p remained virtually constant at 01%, but with the position angle rotating smoothly with a period of about 14 days The same star also exhibited circular polarization of about 1%, but the data were insuf cient to reveal periodicity, if any Subjecting these data on the star s photometric period of 2d 7, or on its harmonic (1d 35), an exercise not reported in the paper, provides phased curves with no structure, suggesting that the variations are not related to the spots co-rotating with the tar and giving rise to the photometric period Elias II & Dorren (1990) discussed the possibility of the star being a binary system, but the polarimetric variation remains an enigma Reports by a Finnish group, including papers by Huovelin, Linnaluoto, Piirola, et al (1985a, 1985b), Huovelin, Saar & Tuominen (1988), Huovelin, Linnaluoto, Tuominen, et al (1989) and Huovelin & Saar (1990), announcing polarimetric variability of solar-type stars, and linked to chromospheric activity, now appear to have been abandoned, the results, particularly those for the U-band, being susceptible to contamination by scattered moonlight In a Workshop Paper, Leroy (1990) discussed the net polarization that can be generated by the plethora of metal lines.

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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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