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A basic stellar polarimeter comprises a modulator and detector system The units are usually mounted within a box for attachment to the telescope This self-contained polarimetric head may provide observer support devices such as retractable transfer optics for inspection of the telescope image prior to the measurements Instruments using photomultiplier detectors require the use of a eld stop or eld-limiting diaphragm, in similar fashion to a regular photometer According to Pospergelis (1965), the eld stop must have a knife edge of strictly circular shape, with minimal re ecting surface at its edge The aperture should be made with non-metallic material such as ebonite, and the beam must pass through the hole symmetrically If these conditions are not met, spurious linear polarization of up to 01% may arise The simplest form of modulator is a rotatable polarizer prior to a detector As described at the beginning of the chapter, an early polarimeter of this type, used by iltner (1951a), was a standard photometer with a Polaroid inserted whose orientation was adjustable to selected positions In a system described by Hall (1951), a continuous rotating Glan Thompson prism was employed With this instrument, the probable error of the measurements was typically 02%, one of the chief problems being atmospheric intensity scintillation noise A pioneering double-beam polarimeter using a Wollaston prism was constructed by Gehrels & Teska (1960) The output signals for the two channels with photomultiplier detectors were simply recorded by DC ampli ers and pen recorder systems An early design of double-beam polarimeter was also used by Serkowski & Chojnacki (1969) The system comprised a Wollaston prism, with further separation of the resolved components by the apex of an aluminized 97 prism The instrument was rotatable in steps of 45 on the telescope mounting plate Signals were obtained from photomultipliers illuminated via Fabry lenses so that the telescope pupil was imaged on them Difference signals were recorded, and detector imbalances were calibrated using a depolarizer Many of the early instruments involving stepped rotation of wave plates or polarizers were controlled by hand As computer control became an eventuality, such operations were performed by using stepper motors An early automated system was described by Kinman & Mahaffey (1974), this being similar to the design of Visvanathan (1972) In order to reduce sky background contamination that is prevalent at high latitude observatories, Piirola (1973, 1975) designed an instrument with built-in compensation Two diaphragms were placed in the focal plane of the telescope and by a mechanical chopping arrangement, the detector was alternatively illuminated by star plus sky background and then just by an equal area of the sky alone; in this way the contaminating signal from the sky was automatically subtracted The same principle was also incorporated by Korhonen, Piirola & Reiz (1984) and Piirola (1988) in a more sophisticated instrument allowing simultaneous ve-band multi-colour observations.

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A synoptic polarimetric study of some 60 Southern Hemisphere peculiar earlytype stars, including Herbig Ae/Be objects, was undertaken by Yudin & Evans (1998) with a view to investigate variability on time scales of minutes hours and days In addition to the presentation of the results, this work provides many references to previous polarimetry of HAEBE stars A study of the Herbig Ae star, AB Aur, was undertaken by Catala, B hm, Donati, et al (1993) Although the lines of Fe II 5018 and He I 5876 were photometrically spectacularly variable, circular polarization in the former line was surprisingly not detected An upper limit of 1 kG was assigned to the photospheric magnetic eld The same star was observed by Beskrovnaya, Pogodin, Najdenov, et al (1995) for short-term spectral and polarimetric uctuations Particularly from the behaviour of the P Cyg-type pro le of H , they demonstrated that there were connections to circumstellar inhomogeneities moving in the envelope Broadband polarimetry showed variations over a few hours and on longer time scales Pontefract, Drew, Harries, et al (2000) later performed spectropolarimetry at H for this star and found that there is an intrinsic linear polarized emission component suggesting scattering in a rotating circumstellar disc The ocus in the q u-plane of the measurements across the emission pro le displayed a loop (see Figure 139). Make ANSI/AIM Code 128 In Visual Basic .NET Using Barcode creation for .Related: Intelligent Mail Generating .NET

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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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