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1 Introduction and History Parsons, W (1878) (The 3rd Earl of Rosse) Preliminary Note on Some Measurements of the Polarization of the Light coming from the Moon and from the Planet Venus Sci Proc R Soc Dublin, 1, 19 20 [16] Pye, D (2001) Polarised Light in Science & Nature Institute of Physics Publishing, Bristol [26] Schwarz, H E (1984) Spectropolarimetry of cool giants and supergiants PhD Thesis, Department of Astronomy, University of Glasgow [20] Secchi, A (1860) Letter from the Rev Father Secchi to the Astronomer Royal MNRAS, 20 70 71 [16] Semel, M (2003) Spectropolarimetry and polarization-dependent fringes A&A, 401, 1 14 [11] Serkowski, K (1970) Intrinsic polarization of early-type stars with extended atmospheres ApJ, 160, 1083 1105 [21] Serkowski, K (1971) Polarization of variable stars pp 11 31 in New Directions and New Frontiers in Variable Star Research, IAU Colloquium No 15, Bamberg [20, 21] Serkowski, K (1973) Interstellar polarization pp 145 152 in Interstellar Dust and Related Topics IAU Symp No 52 (eds JM Greenberg and HC van de Hulst) Dordtecht, The Netherlands [20] Shakhovskoi, NM (1963) Polarization observations of Lyrae Sov Astron, 6, 587 589 [21] Shakhovskoi, NM (1965) Polarization in variable stars II clipsing binaries Sov Astron, 8, 833 842 [21] Shakhovskoi, NM (1969) The spatial orientation of the orbit planes of close binary stars Sov Astron, 13, 303 305 [21] Shulov, OS (1967) Polarimetric observations of close binary stars Trudy Astron Obs Leningrad, 24, 38 53 [21] Shurcliff, WA (1962) Polarized Light Harvard University Press, Harvard [26] Sten o, JO (1996) Scattering physics Sol Phys, 164, 1 20 [16] Sten o, JO, Keller, CU (1997) The second solar spectrum A new window for diagnostics of the Sun A&A, 321, 927 934 [16] Struve, O, Zebergs, V (1962) pp 368 372 in Astronomy of the 20th Century MacMillan, New York [17] Swindell, W (1975) Polarized Light Benchmark Papers in Optics/1 Dowden, Hutchinson & Ross, Stroudsburg, PA, USA [3, 26] Tapia, S (1977) Discovery of a magnetic compact star in the AM Herculis/3U 1809+50 System ApJ, 212, L125 L129 [22] Thiemann, W (1975) Life and Chirality Beyond The Earth Origins of Life, 6, 475 481 [25] Thiessen, G (1961) ber die Polarisation des Sternlichtes, die Strahlung der Sterne, Sowie Bemerkungen zur Galaktiscehn Struktur Astr Abh Hamburg Stern, Vol V, No 9 [21] Tinbergen, J (1996) Astronomical Polarimetry Cambridge University Press, Cambridge [26] Trujillo-Bueno, J, Moreno-Insertis, F, S nchez, F (2001) Astrophysical Spectropolarimetry Cambridge University Press, Cambridge [26] Turner, G (1957) Nineteenth-century studies of the polarization of light re ected by the Moon JBAS, 67, 185 188 [16] Turner, G (1958) The polarization of light re ected by the lunar surface JBAS, 68, 253 263 [16] Umov, N (1912) Eine spektropolariskopische Methode zur Erforschung der Lichtapsorption und der Natur der Farbstoffe Phys Zeitschr, 13, 962 971 [16] Walker, J (1978) More about polarizers and how to use them particularly for studying polarized sky light Scienti c American, 238, 132 136 [3] Whittaker, E (1958) A History of the Theories of Aether and Electricity Thomas Nelson, London ( rst published 1910, Reprinted 1958) [9, 10] Wolstencroft, RD (1985) The search of extra-terrestrial life: recent developments pp 171 175 in Astronomical Sources of Circularly Polarized Light and Their Role in Determining Chirality on Earth IAU Symp No: 112, Boston 18 21 June 1984 Ed MD Papagiannis, Reidel, Dordrecht [25] Zellner, BH, Serkowski, K (1972) Polarization of light by circumstellar material PASP, 84, 619 626 [21].

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indexed by a parameter For random variable , write P . Maker In Visual C#.NET Using Barcode encoder for VS .Photon counts Light intensity from a single source varies with time, and is usually assumed to be normally distributed However, quantum mechanics interprets measurements of light intensity as photon counting Ordinary light sources that produce light by thermal emission should ollow a Poisson distribution or Bose Einstein distribution on very short time scales On longer time scales (longer than the coherence time), the addition of independent variables yields an approximately normal distribution The intensity of laser light, which is a quantum phenomenon, has an exactly normal distribution Measurement errors Repeated measurements of the same quantity are expected to yield results which are clustered around a particular value If all major sources of errors have been taken into account, it is assumed that the remaining error must be the result of a large number of very small additive effects, and hence normal Deviations from normality are interpreted as indications of systematic errors which have not been taken into account Note that this is the central assumption of the mathematical theory of errors A13212 Cauchy Distribution The Cauchy distribution is an example of a continuous distribution that does not have an expected value or a variance In physics it is usually called a Lorentzian, and it is the distribution of the energy of an unstable state in quantum mechanics In particle physics, the extremely short lived particles associated with such unstable states are called resonances The Cauchy distribution has the probability density.Related: .NET EAN-13 Generating , Generate EAN 128 .NET , Create UPC-A .NET

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13 Early-type Stars GC, Hutter, DJ, Pauls, TA, Lester, JB (2003) A method for internal calibration of optical interferometer data and application to the circumstellar envelope of Cassiopeiae AJ, 125, 3378 3388 [286] Vakili, F, Mourard, D, Stee, Ph, Bonneau, D, Berio, P, Chesneau, O, Thureau, N, Morand, F, Labeyrie, A, Tallon-Bosc, I (1998) Evidence for one-armed oscillations in the equatorial disk of Tau from GI2T spectrally resolved interferometry A&A, 335, 261 265 [286] Fox, GK (1993a) The scattering of polarized radiation through optically thin circumstellar envelopes MNRAS, 260, 513 524 [290, 290] Fox, GK (1993b) A polarimetric investigation of a magnetically driven Be star wind MNRAS, 260, 525 528 [290] Fox, GK, Brown, JC (1991) Stellar occultation of polarize light from circumstellar electrons: II Flat envelopes viewed at arbitrary angle ApJ, 375, 300 313 [289] McLean, IS (1979) Interpretation of the intrinsic polarizations of early-type emissionline stars MNRAS, 186, 265 285 [292] McLean, IS, Brown, JC (1978) Polarisation by Thomson scattering in optically thin stellar envelopes III A statistical study of the oblateness and rotation of Be star envelopes A&A, 69, 291 296 [289] Nordsieck, KH, Babler, B, Bjorkman, KS, Meade, MR, Schulte-Ladbeck, RE, Taylor, MJ (1992) Stellar Spectropolarimetric Monitoring at The University of Wisconsin pp 114 117 in Nonisotropic and Variable Out ows from Stars ASP Conf Ser, No: 22, (eds L Drissen, C Leitherer & A Nota), San Francisco [287, 288] Poeckert, R, Marlborough, JM (1978a) A model for Cassiopeiae ApJ, 220, 940 961 [292] Shakhovskoi, NM (1965) Polarization in variable stars II clipsing binaries Sov Astron, 8, 833 842 [287] Vink, JS, Harries, TJ, Drew, JE (2005) Polarimetric line pro les for scattering off rotating disks A&A, 430, 213 222 [293] Wood, K, Bjorkman, JE, Whitney, BA, Code, AD (1996a) The effect of multiple scattering on the polarization from axisymmetric circumstellar envelopes I Pure Thomson scattering envelopes ApJ, 461, 828 846 [291] Wood, K, Bjorkman, JE, Whitney, BA, Code, AD (1996b) The effect of multiple scattering on the polarization from axisymmetric circumstellar envelopes II Thomson scattering in the presence of absorptive opacity sources ApJ, 461, 847 857 [291] Wood, K, Bjorkman, KS, Bjorkman, JE (1997) Deriving the geometry of Be star circumstellar envelopes from continuum.