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The temporal variation of p ( ) of R CrB itself was observed by Coyne & Shawl (1973) during a photometric minimum Very signi cant developments in the spectral behaviour were recorded, these being interpreted as dramatic changes in the distribution of particles of different sizes associated with the discrete cloud model Further observations were presented by Coyne (1974), which supported the model Spectropolarimetric observations have been made of V 854 Cen by Kameswara Rao & Raveendran (1993) They noted that the p ( ) variation was much steeper during the light minimum During the brightness decline phase, the polarized ux was attenuated by the same factor as the ux directly from the star, this implying that the obscuring cloud affects both the radiation from the photosphere and the scattering centres, suggesting a restriction to the geometrical extent of the scattering region In an observational study of the global values of p in a collection of objects in the stages of evolution from red giant to planetary nebula, Johnson & Jones (1991) noted that polarization is a characteristic of the majority of these stars When arranged on an evolutionary sequence, a clear trend in p was found A maximum of polarization was observed within an evolutionary stage The value of p was found to increase with age from mildly dusty Mira variables, through to protoplanetary nebulae for which the highest polarization is found; the polarization then decreases as the star evolves into an old planetary nebula Spectropolarimetry of 31 post-asymptotic giant branch (post-AGB) stars were observed by Trammell, Dinerstein & Goodrich (1994), these objects believed to be in the rst phases of the transition from the AGB to the planetary nebula stage Their survey suggested that the objects might be placed into one of four types depending on the recorded behaviour of p ( ) and ( ) Type [1] objects display higher levels of polarization and large position angle rotations; Type [2] have polarizations too large to be attributed to interstellar material, but without large position angle changes; Type [3] objects show position angle rotations nd polarization changes across TiO absorption features; Type [4] are objects for which the observed polarization can be entirely attributed to interstellar effects Twenty four objects displayed evidence for aspherical geometry, with an implication that asymmetry begins very early in the transition from AGB to the planetary nebula phase Their schematic model involves bipolar lobes giving rise to polarization in the blue part of the spectrum as a result of scattering of photospheric light by the contained dust grains Orthogonal to these lobes is an obscuring torus, and the polarization in the red is the result of scattering of photospheric light or transmission polarization in this torus Likkel, Morris, Kastner, et al (1994) have obtained maps of IRAS 21282+5050 revealing that the polarization is not centro-symmetric close into the stellar source It was concluded that there is not a large component of scattered light in the nearinfrared The emission at 22 m may arise from transiently heated dust In a polarimetric study of IRC +10216, a carbon-rich infrared evolved star on the AGB of the HR diagram, Kastner & Weintraub (1994) found elliptical symmetry in a J-band map endorsing other photometric maps, all these providing evidence of axial symmetry of the envelope, with the equatorial plane of the star lying perpendicular to the major axis of the surrounding inner envelope of the nebula The axisymmetric.

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region of star formation The forms of the p ( ) curves are also indistinguishable from those describing the general interstellar medium The polarization data are used to determine polarization-to-absorption ratios, and to make better estimates of the distance, size and mass of the cluster The Pleiades have also been studied in combination with reddening effects Using UBV lters, Markkanen (1977b) measured 12 of the brighter stars and found that the position angles coincided with the lament directions of the nebulosity Several of the stars showed indications of intrinsic polarization, Pleione exhibiting a growth in p during the observations Later measurements by Breger (1984) failed to con rm suspicions in the literature concerning a high incidence of intrinsic polarization He found that the polarization/extinction ratio was compatible with an interstellar origin A set of stars suspected as being pre-main-sequence was examined by Breger (1985) He was unable to con rm previously reported abnormal wavelength dependencies of polarization; the high polarization values of some faint stars were shown to be caused by high interstellar reddening in the molecular cloud region southwest of Merope Based on polarimetry, 10 suspected pre-main-sequence stars were explored to see if their apparent high reddening, causing their abnormal positions in the HR diagram, could be related to interstellar material For nine of the candidates, the determined interstellar reddening could not account for their offset from the main sequence A more complete picture of the polarimetry of the Pleiades was given by Breger (1986), with the measurements being linked to colour measurements and millimetre and radio data From the eastern part of the cluster, the interstellar material is uniform, resulting in constant values of p (V ) D 027%, D 114 , E(B V ) D 003 mag, the region coinciding with a 21 cm HI minimum Light from the northwestern part passes through the foreground material in addition to a patchy intracluster cloud, and depolarization occurs due to the different magnetic eld directions in the two clouds A high reddening of 030 mag and polarization 2% in much of the southwestern region coincides with the position of a O molecular cloud Corso, Shatzel, Lange, et al (1993) have described a photographic survey and CCD technique for measuring stars with high polarization in the x Cas region The average value of p is between 3 and 5%, with a few stars in excess of 6% There is a tendency for the stars of highest polarization to occur south of the galactic equator in this region Determination of the intracluster polarization properties of the dust in the Carina nebula was reported by Marraco, Vega & Vrba (1993) In combination with photometric data, colour polarization measurements were modelled in terms of a foreground interstellar component which was then subtracted to provide intracluster values It was concluded that the latter were generated with lower ef ciency relative to the interstellar medium The intracluster dust was characterized by a ratio of E(V K) /E(B V) to max higher than the canonical value for the interstellar medium The reddened open cluster, NGC 1502, has been studied by Weitenbeck, Halstead & Carver (2008) The polarization grows from being less than 1% at a distance of 100 200 pc to over 6% for the cluster stars; the directions of vibration are uniform.

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