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Stellar P larimetry McLean, IS (1980) Periodic variations in the linear polarization of HD 50896: A new Wolf Rayet binary ApJ, 236, L149 L153 [299] McLean, IS, Coyne (SJ), GV, Frecker, JE, Serkowski, K (1979) Detection of polarization structure across the emission lines of the Wolf Rayet star HD 50896 ApJ, 231, L141 L145 [299] Moffat, A, Piirola, V (1993) Polarization variability among Wolf Rayet stars VIII Emission lines versus continuum in WR + O binaries ApJ, 413, 724 734 [299] Piirola, V, Linnaluoto, S (1988) Multicolour Polarimetry of Wolf Rayet binaries pp 655 666 in Polarized Radiation of Circumstellar Origin Vatican Observatory Conference Proceedings: (eds GV Coyne, AM Magalh es, AFJ Moffat, RE Schulte-Ladbeck, S Tapia & DT Wickramasinghe) University of Arizona Press, Tucson, AZ [300, 300] Richardson, LL, Brown, JC, Simmons, JFL (1996) Polarimetric versus photometric variability and the density of WR star wind inhomogeneities A&A, 306, 519 526 [302] Robert, C, Moffat, AFJ (1989) Polarization variability among Wolf Rayet stars IV A complete lack of circular polarization in the optical continuum ApJ, 343, 902 908 [302] Robert, C, Moffat, AFJ, Bastien, P, Drissen, L, St-Louis (1989) Polarization variability among Wolf Rayet stars V Linear polarization of the bright Cygnus stars and an anticorrelation with wind speed ApJ, 347, 1034 1054 [302] Robert, C, Moffat, AFJ, Bastien, P, St-Louis, N, Drissen, L (1990) Polarization variability among Wolf Rayet stars VI Linear polarization of the eclipsing binary V 444 Cygnii ApJ, 359, 211 218 [300] Rudy, RJ, Kemp, JC (1978) A polarimetric determination of binary inclinations ApJ, 221, 200 210 [300] Schulte-Ladbeck, RE (1989) Masses and the evolution of Wolf Rayet binaries AJ, 97, 1471 1479 [299] Schulte-Ladbeck, RE, Nordsieck, KH, Nook, MA, Magalh es, AM, Taylor, M,Bjorkman, KS, Anderson, CM (1990) A rotating, expanding disk n the Wolf Rayet star EZ Canis Majoris ApJ, 365, L19 L22 [299] St-Louis, N, Drissen, L, Moffat, AFJ, Bastien, P, Tapia, S (1987) Polarization variability among Wolf Rayet stars I Linear polarization of a complete sample of Southern Galactic WC Stars ApJ, 322, 870 887 [300, 300].

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For binary systems, phased-locked variations can be used to determine some of the basic orbital characteristics such as a value for the inclination, this being very important for resolving the mass function The distribution of scattering material around any system may be established with estimates for the rate of mass loss Schulte-Ladbeck (1989) discussed the importance of knowing the masses of Wolf Rayet binaries in respect of their evolution, and she emphasized the role that polarimetry plays in helping to establish a catalogue of values The appendix of her work provides a summary of 10 such systems For single stars, polarization variability provides information on asymmetries and inhomogeneities (blobs) in the stellar wind As early as 1946, Kopal & Shapley (1946) suggested that the eclipsing Wolf Rayet, V 444 Cyg, was an ideal system for investigation by polarimetry From the light curve, they concluded that the main cause of extinction in the semi-transparent envelope surrounding the WR component is scattering by free electrons, and, in turn, this would produce a small polarized ux best seen several hours before and after primary minimum Monitoring the variation of p should provide an estimate of the proportion of the light scattered, and allow determination of the longitude of the node of the binary system Early polarimetric observations of a WR star were those of McLean, Coyne, Frecker, et al (1979) using a spectral resolution of 50 , revealing that the prominent emission lines of HD 50896 = WR 6 = EZ CMa, a WN5-type star, exhibited decreases of polarization relative to the continuum The behaviour suggested strati cation of ionization and excitation in the extended atmosphere, with the recombination lines of He II being formed deeper than those of He I, so that the ionization is decreasing outwards The continuum polarization is typical of almost pure electron scattering, suggesting that the envelope must be highly ionized and attened to some degree, or localized Later, McLean (1980) showed that the system had a polarimetric period of 1d 88, this being the second harmonic of the 3d 76 value associated with photometric and spectroscopic modulations Determination of i was made dif cult because of aperiodic instabilities, but a value of 71 was suggested, implying a 13 M companion for the 10 M primary star As a result of a photometric and polarimetric campaign, Drissen, Robert, Lamontagne, et al (1989) found that the shapes of both the light curve and the polarimetric curve changed over 2 months, but maintained the periodicity From high spectral resolution measurements, Schulte-Ladbeck, Nordsieck, Nook, et al (1990) revealed that the position angle of the polarization changed across the emission lines such that loops were executed in the q u-plane Such behaviour may be explained in terms of there being a rotating, expanding disc n the system The behaviour of the emission lines was explored further by Moffat & Piirola (1993) who found their polarization variation 03% was very much less than that of the continuum 16% For two other non-eclipsing WC7 + O binaries, they found no variation in the emission complex of C III/IV 4650 + He II 4685 , in.

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sensitivity of an optical element or detector to polarized light The depolarizer designed by Lyot (1929) comprises two thick wave plates made of the same material with their axes set at 45 ; one plate is twice the thickness of the other A typical depolarizer comprises quartz plates of 1 mm and 2 mm thick Over a broad wavelength passband, any polarization present in a beam which it passes is scrambled both in polarization form and direction of vibration The ef ciency to which this is done has been explored comprehensively by Serkowski (1974) For narrow spectral passbands the scrambling process of the Lyot depolarizer is insuf cient for it to be effective In such a situation, an alternative principle relies on the notion of performing the scrambling with respect to time, the resulting output polarization changing rapidly within the experimental integration interval of the measurement Several monochromatic depolarizers were suggested by Billings (1951) One of them, involving the rotation of a quarter-wave plate followed by a half-wave plate rotating at twice he speed of the rst, was tested by Clarke & Ameijenda (2000) Although successful, the system was subject to image wobble as a result of the wave plate surfaces not being exactly normal to the rotational axis. Bar Code Generator In Visual Studio .NET Using Barcode creator for VS .NET Control to .Related: C# ISBN Generating , .NET WinForms EAN-8 Generation , Java Code 128 Generating

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