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WAS is automatically installed in Vista and Windows 2008 when IIS is installed, because IIS is dependent on it When IIS is installed, it registers w3svc as an HTTP listener adapter with WAS When NET 35 is installed, it registers listener adapters for TCP, MSMQ, and named pipes with WAS It s also possible to use WAS without installing IIS To do his, you must enable two Windows features First, you must enable the Windows Process Activation Services as shown in Figure 72 You get to this screen in. GS1 128 Creator In Java Using Barcode drawer for . Windows by clicking Start, Control Panel, Programs, Turn indows Features On or Off .Related: Generate Intelligent Mail Excel , PDF417 Generation Excel , UPC-E Generating ASP.NET

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taining solid particles Both NML Cyg and VY CMa display circular polarization in the infrared as described by Serkowski (1973) Maximum v occurs near the wavelength of minimum linear polarization, as expected from Mie scattering theory VY CMa may be classi ed as a hypergiant Being the largest known star, and also one of the most luminous, it has attracted much observational attention as an OH emission source Large polarization was detected by both Shawl (1969) and Serkowski (1969a), together with a strong wavelength dependence of the position angle The UBV measurements suggested that Rayleigh scattering by circumstellar dust grains produces the polarization, rather than synchrotron radiation being present Hashimoto, Maihara, Okuda, et al (1970) made observations of this object in the infrared H- and K-bands nding the values to follow an extrapolation of measurements made previously by others in the visual part of the spectrum Forbes (1971) extended the polarization measurements of VY CMa into the infrared, con rming a near-linear rise of p with wavenumber Extremely high values of polarization in the blue spectrum region have been observed by Serkowski (1969b) in the nebulae associated with VY CMa and R CrA For the former object, the value of p was 40% Both stars also showed signi cant changes in p over an interval of a few weeks By exploring the polarization structure associated with the nebulosity surrounding VY CMa, Herbig (1972) suggested that the temporal variability of the integrated radiation can be explained by the photometric variability of the star, or of portions of the nebula The dispersion of the polarization position angle can be explained by a wavelength variation of the relative brightness of the star and various parts of the nebula Remarkable structure in the spectral range 4000 8250 , with reductions in p 1% and rotations of direction of vibration 10 across the TiO bands, have been recorded by Aspin, Schwarz & McLean (1985) for VY CMa Using a cell hotspot model , they reproduced the characteristics of the observed behaviour, providing possible values for the sizes of the hotspots and their temperatures The difference in behaviour between VY CMa and Ori can be accounted for by an increase in the amount of scattering material, or by taking the effective temperature as 2700 K, compared with 3900 K The Becklin Neugebauer (BN) object in the Orion nebula has also attracted polarimetric attention Breger & Herdorp (1973) made observations at 16 m and found a polarization of 25% In addition, they also investigated NU Ori, also near to the Orion Nebula, with a range of passbands, and noticed that there was a signi cant rotation of the position angle across the spectrum Loer, Allen & Dyck (1973) extended the infrared polarization measurements of the BN object to 22 and 35 m The polarization displayed a minimum between 4 and 8 m encouraging circular polarization measurements to be attempted by Serkowski & Rieke (1973) with positive results Some part of the polarization appears to have its source in a dense cloud, with mean alignment of particles changing along the line of sight Dyck, Capps, Forrest, et al (1973) found this same object to be ighly polarized in the 5 11 m spectral range From 8 to 11 m, the polarization is strongly correlated with the optical depth in the 10 m absorption feature, and reaches a maximum of about 15% at 10 m The observations are consistent with the polarization being.

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