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for all the Miras Little or no line effects were noted for R Sct An example of these data is presented in Figure 142 for R And Using narrow-band lters to isolate strong features such as the TiO bands and the CaI line at 4226 , Codina-Landaberry & Magalh es (1980) have observed four Miras in the Southern Hemisphere, and the semi-irregular variable L2 Pup Variability was found in the TiO bands in all of the target stars The behaviour is thought to be controlled by the variation of the source function, and the ratio of absorption to scattering, as a function of optical depth in the stellar photosphere For L2 Pup, there were polarization changes across the calcium line, indicating that CaI is unevenly distributed across a stellar surface Further narrow-band measurements were made of L2 Puppis by Magalh es, Coyne, Codina-Landaberry, et al (1986) over a 3-year period Systematic changes were recorded in both p and , being most noteworthy for the CaI 4226 atomic line The behaviour was best explained by a combination of photospheric effects including a non-uniform distribution of Ca across the stellar disc, and scattering from dust grains in an asymmetric cloud about the star, in which there is a systematic time variation in grain size with distance from the star A sample of Mira-type variables was onitored by Boyle, Aspin, Coyne, et al (1986) with 20 resolution over the blue end of the spectrum The most remarkable feature of the study was the behaviour of the resonance line, CaI 4226 Many of the surveyed stars, but not all, showed enhanced p in this atomic line, with several revealing rotation of the direction of vibration relative to measurements of the nearby continuum For some stars, there is a decrease in p across the TiO bands, whereas for others there is an increase It is argued that these behavioural features require more than one polarigenic mechanism, and that both photospheric and circumstellar processes are important Spectropolarimetric studies have been made by Bieging, Schmidt, Smith, et al (2006) for a selection of asymptotic giant branch (AGB) and post-asymptotic giant branch stars Most of the objects exhibited intrinsic polarization with features being detectable in the various molecular lines Effects were recorded in the TiO bands of three M-type Mira variables, in the CN bands of the carbon stars R Lep and V 384 Per, and in the Swan bands of C2 in R CrB and two proto-planetary nebulae Polarization effects in the molecular bands appear to be more common, and the effects are larger, in O-rich rather than C-rich objects.

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Method FromArgb FromKnownColor FromName GetBrightness GetHue GetSaturation ToArgb ToKnownColor Description Creates a Color structure from the four 8-bit ARGB component (alpha-red reen-blue) values Creates a Color structure from the specified predefined color Creates a Color structure from the specified name of a predefined color Returns the hue-saturation-brightness (HSB) brightness value of this Color structure Returns the HSB hue value, in degrees, of thisColor structure Returns the HSB saturation value of thisColor structure Returns the 32-bit ARGB value of this Color structure Returns the KnownColor value of this Color structure.// Create a new Point object Point pt = new Point(50, 50); // Create a new point using PointEmpty Point newPoint = PointEmpty; // Set X and Y properties of Point newPointX = 100; newPointY = 200; // Create a Graphics object from the // current form's handle Graphics g = GraphicsFromHwnd(thisHandle); // Create a new pen with color blue // and width = 4 Pen pn = new Pen(ColorBlue, 4); // Draw a line rom point pt to // new point gDrawLine(pn, pt, newPoint); // Dispose of Pen and Graphics objects pnDispose(); gDispose(); Figure 210 shows the output of Listing 23 The program draws a line from point 1 to point 2 The "Point" text in this figure is a menu item. Barcode Generation In Visual C# Using Barcode generation for VS .Related: Generate ISBN Java , QR Code Generating C# , Create Intelligent Mail C#

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GS1-13, EAN/UCC-13 A European Article Number (EAN) is . It is also known as European Article Number 13, EAN-13 Supplement 5/Five-digit Add-On, EAN-13 Supplement 2/Two-digit Add-On, EAN-13+5, EAN-13+2, EAN13, EAN13+5, EAN13+2, UPC-13, GTIN-13, GS1-13, EAN/UCC-13 A European Article Number (EAN) is a barcoding standard which is a superset of the original 12-digit Universal Product Code (UPC) system developed in orth America. The EAN-13 barcode is defined by the standards organisation GS1. It is also called a Japanese Article Number (JAN) in Japan. UPC, EAN, and JAN numbers are collectively called Global Trade Item Numbers (GTIN), though they can be expressed in different types of barcodes. .Related: Barcode Generation SSRS C# , Barcode Generator SSRS , Barcode Generator RDLC

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minimum brightness, while others were least polarized at maximum brightness From simultaneous photometry and polarimetry of 21 late-type stars, Dyck (1968) found that, for the Mira variables, there was a correlation between changes in brightness and p; an increase in brightness corresponds to a decrease in p, and vice-versa Immediately following the discovery of intrinsic Mira polarizations, Donn, Stecher, Wickramasinghe, et al (1966) proposed that the polarigenic mechanism was graphite dust, this being very ef cient in its effect A further study by Dyck & Sanford II (1971) of 21 Mira variables generally showed the large increase of polarization in the blue end of the spectrum indicating that it must originate in the circumstellar envelope, rather than in the stellar atmosphere Shawl (1975b) later presented data for 25 red variables and discussed models which suggest that a large number of small particles are produced with each light cycle, but growing in size on dispersion For o Cet and V CVn, the polarization increases at the time when the hydrogen emission lines become visible From a study by Materne (1976) of three Miras, whose intrinsic polarizations were corrected for interstellar effects, it was concluded that, following the triggered eruption of small particles, the grain size grows as they disperse, thus con rming Shawl s study Hayes & Russo (1981) noted that the position angles at maximum light of o Cet differ greatly from cycle to cycle; some further measurements have been provided by Hayes (1982) Synoptic multi-colour measurements of three Miras have been made by Yudin & Evans (2002) They suggest that the polarimetric variability which is more evident in the blue, rather than in the more stable red end of the spectrum, is consistent with episodic mass ejections with the formation of small dust particles in the circumstellar environment Attempts to detect circular polarization in a sample of late-type stars was ade by Rich & Williams (1973), with a possible detection only for the star Z Eri For the others including o Cet, null results were obtained Circular polarization had previously been recorded in VY CMa (04% at 1 m, < 05% with a V lter) by Gehrels (1972), and in NML Cyg (maximum, 06% at 17 m) and VY CMa by Serkowski (1973) Narrow- and intermediate-band measurements were made by Coyne & Magalh es (1977) of a number of Mira variables and also the semi-irregular variable, V CVn They suggested from the increase in p around H , and the relative decrease near the Balmer discontinuity, any polarizing dust must be well mixed in the extended atmosphere of the latter star, and that the behaviour may be explained by a shock wave passing through the envelope Further observations by Coyne & Magalh es (1979), particularly of the TiO bands of Cep and V CVn, con rm the model of a pulsating molecular scattering atmosphere in which the polarization is linked to the pulsation cycle, and the polarization changes across the TiO bands are due to changes in the ratio of absorption to scattering with optical depth By using narrow-band lters, McLean (1979) supported the discovery that longperiod (regular) variable stars exhibited signi cant linear polarization variations across some of their molecular bands and atomic lines Variations in p and position angle were found across the stronger molecular (TiO) absorption bands in the yellow and red spectral regions of Cep and R Tri.

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