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During the period when an interstellar origin for the polarization was being rmly established, Thiessen (1961) proposed that the polarigenic mechanism was intrinsic to the stellar atmosphere and generated partly by synchrotron radiation His thesis was discussed by Struve (1961) who noted that the proposal would drastically change the current theories of stellar structure Although Behr (1961) showed that the foundations of Thiessen s arguments were erroneously based on observational selection, a repost was presented by Thiessen (1962), this being published after his tragic death It may be noted that Thiessen s predicted variability of polarization in magnetic stars was observed by him for HD 71866 Cernuschi, Marsicano & Kimel (1965) have studied the evolution of stellar matter resulting from supernovae explosions with the resulting grains developing a large magnetic moment Under the local conditions, pairs of spherical grains may coalesce, to produce ellipsoidal particles Their scenario, in terms of the produced numbers of particles, and the fraction which are orientated by the magnetic eld, is tenable in relation to observed values of interstellar polarization As for the mechanism by which the elongated grains are preferentially aligned, there have been several proposals, none of which is perfectly satisfactory Those which require the presence of a magnetic eld have special appeal as the polarization vector maps provide interpretations of galactic magnetic eld structures The issues related to the various proposed mechanisms have been presented by Lazarian (2003) This reference summarises the the roles of the various players in alignment theory including paramagnetic dissipation experienced by rotating grains (Davis reenstein process), mechanical alignment by bombarding atoms (Gold process), and radiative torques (Dolginov process) His thesis promotes the notion that the latter mechanism was not fully appreciated when it was rst suggested some 25 years ago, but is now a strong contender for being the chief process whereby grains are aligned Lazarian & Cho (2005) claim that the bulk of existing observational data related to molecular clouds is consistent with the radiative torque alignment mechanism The Davis Greenstein mechanism (see Davis & Greenstein, 1951) requires the grains to have paramagnetic properties The interstellar eld, say with the ux denE sity B, induces a eld within the particle, the strength depending on the magnetic susceptibility In a static situation, the internal and external elds would be parallel For a spinning grain, however, adjustment of the internal eld lags so that there is.

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expected net polarization, while at high inclination, the polarization is reduced by occultation Their analysis was also applied to the variation of polarization from binary systems in which the scattering material consists of a rotating onedimensional plume etween the stars, superposed on an axisymmetric disc They showed that the inclination of the system and the radial structure of the plume can be deduced for suf ciently high inclinations (i > 60 ) The extent to which the method can be generalized to an arbitrarily distributed two-dimensional scattering region was considered via Fourier analysis It was found that the inclination of the system is largely insensitive to the density distribution when the distribution function is of a simple power-law form The question was also raised that for some stars, the polar mass loss will have a greater ionization fraction than the equatorial region, such that the pole might be the dominant source for free electrons In the third paper of this series, Fox (1991) considered the effects of occultation and nite sized-source depolarization, concluding that the net polarization has a complicated inclination dependence, and that the simple result of it being p / sin2 i, obtained by Brown & McLean (1977), does not hold For Be stars with high intrinsic polarizations, the circumstellar envelope must be concentrated either towards equatorial or polar regions, and that a substantial optical depth is required with > 005 The possible variability of the observed polarization from an obliquely rotating envelope has been investigated by Fox (1992), such a scenario having been mooted by others as being an alternative interpretation to diagnoses involving binary motion, but with lack of spectroscopic evidence to add weight to such duplicity The results of the exercise were not too sanguine as it was evident that effects due to rotation about a body axis and binary orbital motion are indistinguishable It was also found that the physical geometry of the obliquely rotating envelope could not be inferred When the light source is considered to have nite extent, discrimination between envelope geometries emerges to some degree as a result of the occultation of parts of the envelope by the extended source Further modelling by Fox (1993a) has emphasized the effect that an extended light source has on the resulting polarization by scattering in circumstellar envelopes If the underlying star is non-spherical, as a result of its large rotational velocity say, its photosphere will also generate a net polarization, adding to that which is produced by scattering within the extended atmosphere This situation has been modelled by Fox (1993a) who found that, in general, the predicted polarization was a factor of 2 3 times larger than what is observed for Be star systems It was also noted that the theoretical models for Be star envelopes had not yet reached a level of sophistication to estimate by polarimetry the number density of free electrons throughout the circumstellar envelope The origin of stellar winds in Be stars may be in uenced by magnetic elds and Fox (1993b) has considered this additional parameter in polarimetric models From his analysis, the range of observed values of p can be explained if the stars possess small magnetic elds of B0 < 100 G Observed increases in p during the onset of a shell phase is indicative of an increased magnetic eld.

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