Polarimetric Spectral Behaviour in .NET framework

Generate Code 3 of 9 in .NET framework Polarimetric Spectral Behaviour
1321 Polarimetric Spectral Behaviour
Scan Code 3 Of 9 In Visual Studio .NET
Using Barcode Control SDK for VS .NET Control to generate, create, read, scan barcode image in .NET applications.
In a survey of the wavelength dependence of polarization, Coyne & Gehrels (1967) found several early-type stars with variable polarization, while a new tool in identifying early-type stars with intrinsic polarization was introduced by Serkowski (1968), and later extended by him (see Serkowski, 1970 and Figure 131) He found that emission-line stars exhibit a peculiar wavelength dependence of polarization,
Code39 Generation In .NET Framework
Using Barcode generator for VS .NET Control to generate, create Code 39 image in .NET applications.
13 Early-type Stars
Recognizing Code 3 Of 9 In Visual Studio .NET
Using Barcode reader for Visual Studio .NET Control to read, scan read, scan image in .NET framework applications.
Fig 131 A plot of p U /p B against p V /p B clearly distinguishes the intrinsic polarization associated with Be stars (C) relative to stars exhibiting interstellar polarization ( ) which occupy a band in the upper part of the diagram (After Serkowski, 1970)
Paint Bar Code In VS .NET
Using Barcode printer for VS .NET Control to generate, create barcode image in VS .NET applications.
with low values in the ultraviolet with respect to the average interstellar p ( ) curve Using a series of broadband lters, Coyne & Kruszewski (1969) and Coyne (1971a) observed the p ( ) curve in the region of 3000 10 000 in 19 Be stars Although it was realized that interstellar polarization in uenced some of the measurements, no real effort was made to remove its effects from the recorded values With an observed anti-correlation of the p ( ) curve with the bound-free absorption coef cient of hydrogen, and with dips in the polarization at the Balmer and Paschen limits being a fairly common feature, it was immediately apparent that the behaviour could be attributed to electron scattering in an asymmetric circumstellar cloud, modi ed by polarized radiation from hydrogen recombination and by hydrogen bound-free opacity Poeckert & Marlborough (1976) observed the linear polarization of 48 Be stars in two-colour bands near the H line, with the aim of exploring the relationship between the intrinsic p and v sin i It was found that intrinsic polarization depends strongly on v sin i; stars with low v sin i displayed little, or no, polarization No apparent difference between pole-on and extreme Be stars was obtained It was found that from the relationship between the intrinsic p and v sin i, and assuming thin discs, an envelope density of 5 1011 cm 3 can account for the levels of polarization recorded for all of their observed stars A review of the status of the polarization associated with Be stars at the time of the mid-1970s was presented by Coyne (1976a) A review of studies of polarimetry of Be stars up to the early 1980s was presented by Coyne & McLean (1982)
Read Barcode In Visual Studio .NET
Using Barcode scanner for .NET framework Control to read, scan read, scan image in Visual Studio .NET applications.
Stellar P larimetry
Generate Code 3/9 In Visual C#.NET
Using Barcode maker for VS .NET Control to generate, create USS Code 39 image in .NET framework applications.
Poeckert, Bastien & Landstreet (1979) conducted an intermediate-band survey of 70 Be stars, reducing their values to remove the contaminations of interstellar polarization About half of the group exhibited intrinsic effects, but there was no single universal wavelength dependence that could be scaled to t all Be stars There were marked variations from star to star at the Balmer jump, and for the slope of the Paschen continuum A logical step in terms of experimental observations was the investigation of the spectral behaviour of the intrinsic polarization in the region of the Balmer emission lines themselves In the very early 1960s, Tamburini & Thiessen (1961) had suggested from some observations of bright stars, including two Be types, that polarizational variations may occur within their spectral lines This work was followed by similar reports by Clarke & Grainger (1965, 1966), but these latter results were prone to misinterpretation as a result of their experimental methodology In 1972, at the Polarimetry Conference in Tucson, Arizona, Clarke & McLean (1974a) reported on a novel way to undertake polarimetric observations of the emission lines of Be stars using tilted narrow-band interference lters Their system was applied to a study of Cas, and it was found that the intrinsic polarization dropped in the H emission feature (see Clarke & McLean, 1974b and Figure 132) This discovery was immediately followed with similar effects observed by Coyne (1974) in the H emission line of another Be star, Tau Further observations of Cas and Tau at H were made by Clarke & McLean (1976) An immediate interpretation was to consider that the emission radiation was unpolarized, and that the reduction of polarization depended on the strength of the emission line For the Be star, 48 Per, despite the Balmer lines being in emission, no substantial polarimetric changes across H were found Further measurements at H and H of several Be stars were discussed by McLean & Clarke (1976) Hayes & Illing (1974) conducted polarimetric studies of the H line of 10 stars, recording a decrease in p at the line centre of Cas, the only one selected as displaying intrinsic polarization Other stars, chosen on the basis of being fast rotators, showed no polarimetric structure across the line Later, Hayes (1975a) recorded a polarization reduction in the H line of Tau, but noted that, in relation to the strength of the emission, and the reduction of p relative to the continuum levels, it could not be ascribed simply to the addition of unpolarized ux Twelve Be stars were measured by Poeckert (1975) for polarimetric structure across the H line Shell stars like Tau were found to exhibit a decrease in polarization which was proportional to the strength of the emission component Stars considered as being pole-on were found to have no signi cant changes in p, nor position angle, across the line Observations of the polarization at H and H were made by Coyne (1976b) of 28 Be stars Twelve exhibited decreased polarization at these wavelengths, these tending to be stars with a shell spectrum or with large v sin i From investigations of Southern Hemisphere Be stars, McLean & Clarke (1979) found that the polarization reductions in H and H had a more complicated behaviour in relation to a simple unpolarized emission-line ux model For Cen, an increase in polarization was found in the cores of H and H , the effect attributed
Drawing Code 39 In .NET Framework
Using Barcode generator for ASP.NET Control to generate, create Code 39 Full ASCII image in ASP.NET applications.
Code 39 Extended Creation In VB.NET
Using Barcode creation for VS .NET Control to generate, create Code39 image in VS .NET applications.
Printing Code 39 Extended In Visual Studio .NET
Using Barcode generation for .NET Control to generate, create Code 39 Extended image in VS .NET applications.
Making Code 93 Full ASCII In Visual Studio .NET
Using Barcode generation for .NET framework Control to generate, create Code 93 Full ASCII image in .NET applications.
Making Data Matrix In Visual Studio .NET
Using Barcode creation for ASP.NET Control to generate, create Data Matrix 2d barcode image in ASP.NET applications.
Reading UPC-A Supplement 5 In .NET
Using Barcode reader for .NET Control to read, scan read, scan image in .NET applications.
EAN / UCC - 13 Drawer In Visual Studio .NET
Using Barcode encoder for ASP.NET Control to generate, create UCC - 12 image in ASP.NET applications.
UCC - 12 Creator In VB.NET
Using Barcode creation for VS .NET Control to generate, create UPC A image in VS .NET applications.