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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 and polarization changes across TiO absorption features; Type [4] are bjects 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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Stellar P larimetry Dyck, HM, Johnson, HR (1969) Chromospheres and polarization in late-type stars ApJ, 156, 389 392 [311] Kruszewski, A, Coyne, GV (1976) Wavelength dependence of polarization XXXI Cool stars AJ, 81, 641 649 [312] Kruszewski, A, Gehrels, T, Serkowski, K (1968) Wavelength dependence of polarization XII Red Variables AJ, 73, 677 687 [311] Schwarz, HE (1985) Narrow band polarimetry of a sample of cool giants and supergiants A&A, 147, 111 114 [312] Schwarz, HE (1986) Polarimetry of cool giants and supergiants Vistas Astron, 29, 253 280 [312] Shawl, SJ (1975) Wavelength dependence of polarization XXVIII Circumstellar scattering: polarization and reddening models AJ, 80, 595 601 [312] Simmons, JFL (1982) Analytic treatment of polarization by arbitrary scattering mechanisms in circumstellar envelopes I Single Stars MNRAS, 200, 91 113 [312] Simmons, JFL (1983) Analytic treatment of polarization by arbitrary scattering mechanisms in circumstellar envelopes II Binary Stars MNRAS, 205, 153 170 [312] Voshchinnikov, NV, Karjukin, VV (1994) Multiple scattering of polarized radiation in circumstellar dust shells A&A, 288, 883 896 [312] Doherty, LR (1986) On the polarization of alpha Orionis ApJ, 307, 261 268 [315] Grigoryan, KA (1958) Polarization observations of Cep Soob Byurakan Obs, 28, 45 48 [313] Hayes, DP (1980) Ordered linear polarization changes in Betelgeuse ApJ, 241, L165 L168 [313, 314] Hayes, DP (1981a) B- lter linear polarization measurements of Cep in the Autumn of 1980 IBVS, No: 1984, Budapest [313] Hayes, DP (1981b) Lower atmosphere changes inferred from variations in Betelgeuse s linear polarization PASP, 93, 752 755 [314] Hayes, DP (1982) Linear polarization of the late-type variable stars Cep and Mira in year 1981 IBVS, No: 2064, Budapest [313] Hayes, DP (1984) Variations of Betelgeuse s optical linear polarization over four consecutive observing seasons: 1974 1983 ApJS, 55, 179 188 [314] Le Borgne, JF, Mauron, N, Leroy, JL (1986) The polarized dust shell around Orionis I New U BV measurements A&A, 168, 211 216 [315] Marcondes-Machado, JA (1987) A model for the intrinsic linear polarization of cool giant and supergiant stars A&A, 188, 131 136 [315] Mauron, N, Le Borgne, JF (1986) The polarized dust shell around Orionis II The silicon fractional condensation, mass-loss rate and grain radius A&A, 168, 217 224 [315] Schwarz, HE, Clarke, D (1984) The polarization of Orionis I: Interpretation of broadband measures A&A, 132, 370 374 [314] Shafter, A, Jura, M (1980) Circular polarization from scattering by circumstellar grains AJ, 85, 1513 1519 [315] Tinbergen, J, Greenberg, JM, de Jager, C (1981) Multicolor linear polarimetry of Betelgeuse and Antares A&A, 95, 215 220 [313] Tuthill, PG (1994) PhD Thesis: Imaging Stars Through the Atmosphere , 4, University of Cambridge, Cambridge [315] Tuthill, PG, Hanhiff, CA, Baldwin, JE (1997) Hotspots on late-type supergiants MNRAS, 285 529 539 [315].

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The history associated with the revelation of interstellar polarization by Hall (1949) and Hiltner (1949) has already been presented in 1 Both Hiltner and Hall continued to make polarimetric observations following their momentous discovery Hall & Mikesell (1949) reported on some 175 measurements of early-type stars They lso attempted to measure circular polarization, but concluded that the polarization form was essentially linear Hiltner (1950) also extended his measurements to the infrared to see how they behaved relative to the photometric interstellar extinction law Both Hiltner and Hall provided catalogues of their measurements and these have been extended by a host of workers (see the last section of 8) As instrumental sensitivities have improved, explorations of the wavelength dependence of interstellar polarization have progressed, and detections of circular polarization have been pursued All these studies have lead to improvements on the large scale, with respect to mapping structures within the Galaxy, and, on the small scale, to the understanding of the properties of interstellar dust grains, of their growth, and the role they play in respect of interstellar chemistry A popular discourse on interstellar polarization has been given by Greenberg (1967) Several citations on the relationship between polarimetry and our knowledge of the interstellar magnetic eld are given in Heiles (1976) For the developments related to the measurements, their basic interpretation and the elements of scattering theory, a resum to 1980 on the usefulness of polarization as a diagnostic for understanding the nature of interstellar dust has been provided by Greenberg (1978). NET Control to generate, create Code 39 Full ASCII image . In Visual Studio .NET Using Barcode maker for .NET .Related: VB.NET UPC-E Generating , Code 39 Printing ASP.NET , Print PDF417 VB.NET

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