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The collected stellar radiation is transferred by the telescope optics to the polarimetric modulator As a result, the initial polarization may be altered before it is measured by the instrument attached at the telescope s focus The most common spurious effect is that any collected unpolarized light becomes weakly polarized The amount of polarization introduced is referred to as the instrumental polarization There may be additional sources contributing to the instrumental polarization other than the telescope mirrors It is usual practice in any observing programme to investigate the instrumental polarization by making measurements of unpolarized standard stars The mean values of the NSPs for these measurements may be represented by q I and u I , and the position of the instrumental polarization can be plotted in a normalized Stokes vector diagram For measurement of other stars, the reduction procedure involves shifting the origin, O, of the measurements to that of the instrumental polarization position, O0 (see igure 55) This is best done by subtracting the offset, q I , u I , from the q, u values of the program stars The process corresponds to a vector subtraction of the instrumental offset by the inversion of the principle of the Additivity Theorem for Small Polarizations (see Section 45) If the source of instrumental polarization is identi able as occurring in the telescope fore-optics, and can be expressed as a Mueller matrix, a more accurate reduction would involve an inversion procedure to obtain revised values according to the elements of this matrix In the simplest case, the matrix would be that of a weak polarizer; in some cases, there may also be a small phase change introduced by the optics and this would need to be incorporated into the matrix (see further discussion in 7) It is also possible that the telescope optics effect a depolarization to any collected polarized light (see Section 74), this being a true reduction of a degree of polarization and not simply a linear-to-circular conversion Depolarization is a dif cult parameter to investigate, the best that can be done is to inter-compare results taken by different instrumental setups If its effects on all the Stokes parameters are known, and are expressible in the form of a Mueller matrix, in principle, any.

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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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