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differential limb darkening A more sophisticated model has been presented by Doherty (1986) suggesting that the polarization behaviour can be explained in terms of the combined effects of Rayleigh scattering in the photosphere and scattering by circumstellar dust in the presence of one or more photospheric hot spots Assessment of models involving asymmetric distributions of circumstellar dust, alignments of dust by the stellar magnetic eld, or photospheric structures was made by Marcondes-Machado (1987) In his proposal, he demonstrated that good ts to data, including wavelength variations of the position angle, could be produced by a model based on paramagnetic grains which are aligned by a stellar magnetic eld, with the grain size and magnetic eld geometry varying with distance from the star, and with the effective stellar radius changing with wavelength Le Borgne, Mauron & Leroy (1986) have performed polarimetry of the resolved dust shell surrounding Ori Using UBV lters, they found that the dust density falls off according to r 2 , and that no signi cant departures in spherical symmetry could be found Further modelling of the situation was undertaken by Mauron & Le Borgne (1986) to explore the rate of mass loss, with values that depend on the grain type solutions which provide satisfactory ts to the measured polarization The possibility that circular polarization may be generated in the immediate dusty nebulosities surrounding late-type supergiants has been promoted through the modelling by Shafter & Jura (1980) Observations in this area appear to be absent, although circular polarization has been detected in some Mira variables (see below) Intrinsic polarizations have been recorded by White, Shawl & Coyne (1984) for 15 out of 39 measured red giants in the globular clusters NGC 5272 (M3) and NGC 6205 (M13) Possible mechanisms for producing the polarization were discussed in terms of dust in circumstellar envelopes, and from photospheric effects such as surface magnetic elds If localized surface brightness variations are the root cause of the polarization for stars such as Ori, then it should be possible to link the observed position angle to rightness maps produced by high-resolution interferometry An attempt to do this has been described by Tuthill (1994) with some success The relationship of polarimetry to the mapping of hotspots has also been mentioned by Tuthill, Hanhiff & Baldwin (1997) Further interdisciplinary observations along these lines are only to be recommended.

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Following a visual brightness increase, Schulte-Ladbeck, Clayton & Meade (1993) undertook spectropolarimetry of the luminous blue variable (LBV) star, AG Car, and the LMC variable, R 127 For AG Car, the position angle of he intrinsic polarization is aligned with a major axis of the ring nebula and perpendicular to the jet In R 127, the polarization is perpendicular to two bright features of the local material These observations provide strong evidence that the asymmetries seen in the surroundings of these LBVs originate in the underlying stars AG Car became the subject of a more detailed paper by Schulte-Ladbeck, Clayton, Hillier, et al (1994) The H emission line pro le exhibits very extended wings that are differently polarized in amount and position angle relative to both the line core and the continuum, suggesting an origin by electron scattering in a dense wind The polarization exhibits large temporal variations indicating signi cant variations in the envelope opacity The general polarization varies along a preferred position angle of 145 , this direction interpreted as a symmetry axis of the stellar wind Its direction is co-aligned with the major axis of the AG Car ring nebula and perpendicular to the star s jet The temporal polarization variability of AG Car was con rmed by Leitherer, Allen, Altner, et al (1994), who also extended the polarimetry of this object into the ultraviolet Schulte-Ladbeck, Leitherer, Clayton, et al (1993) undertook colour lter measurements of R 127 in the Large Magellanic Cloud The polarization at H decreased with respect to the continuum They assumed that H line is recombination dominated, and thus intrinsically unpolarized, so allowing the interstellar polarization to be estimated The intrinsic polarization was determined to be of the order of 1% ! 15%, implying both the presence of copious free electrons and a considerable asphericity in their distribution Parthasarathy, Jain & Bhatt (2000) have made UBVRI measurements of HR Car, and noted large temporal changes in the level of p, and also in the form of p ( ) Spectropolarimetry of this object was also conducted by Clampin, Schulte-Ladbeck, Nota, et al (1995) Changes of polarization across the H emission line were noted Both these papers imply that the scattering material close to the star does not have a spherically symmetrical distribution, and that the behaviour is consistent with the bi-polar geometry imaged by others using a coronographic technique Spectropolarimetry has been undertaken of LBVs in our Galaxy and in the Magellanic Clouds by Davies, Oudmaijer & Vink (2005) They showed that many of their selected objects exhibit polarimetric signatures across the H emission line, indicating that the light from the stars is intrinsically polarized, and that asphericity already exists at the base of the wind Four of the target stars displayed polarization variability with three of them, AG Car, HR Car and P Cyg, providing temporal position angle changes which appeared random Such behaviour can be explained by the presence of strong wind-inhomogeneities, or clumps within the wind Only one star, R 127, exhibited p variations along an intrinsic line, with evidence of axial symmetry, as well as clumpiness However, if viewed at low inclination, and with limited temporal sampling, such a wind would produce a seemingly random polarization of the type observed in the other three stars.