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Let s do a quick demo to show you the ower of query data connections Keep the preview window open as shown in Figure 610 (Or you can minimize the preview window instead) We want to go back and edit the Samplexml le Double-click on the Samplexml le on the desktop to open it for editing, and then remove, say, the last line: the lazy dog After removing that text, save the form Switch back to the form with the data connection as shown in Figure 610, then click the button again Poof, the last item in the bulleted list disappears! You might have noticed that you cannot insert or remove rows in the secondary data source after clicking the button We ll investigate why this is the case, along with a series of other observations, in 7 when we discuss secondary data source binding.We mentioned that choosing XML or Schema for the main data source doesn t lead to creating a data connection This is because the data in the chosen XML file is used simply to create the form template s main ata source (Optionally, it can also provide the form fields default values) Selecting an XML file for the main data source is a one-time operation Likewise, if a XML Schema is selected, it just defines the structure of the data source. NOTE. Barcode Printer In .NET Framework Using Barcode printer for ASP .Related: ASP.NET QR Code Generation , QR Code Generating .NET Image, Generate QR Code .NET Data

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component, and that the recorded values were wholly interstellar, McLean (1976) pursued such an analysis more thoroughly A distance was determined as 114 kpc, thus providing an absolute magnitude at maximum brightness of 10m 1, a value consistent with its temporal photometric behaviour Zellner & Morrison (1971) reported polarimetric colour measurements of the very slow outburst of Nova HR Delphini 1967, and also for Nova Vulpeculae No 1 1968 and Nova Serpentis 1970 For HR Del 1967, after making correction for its interstellar component, p was 06% in the red during the rst 120 days following the outburst In the later phases, the intrinsic component was generally small and irregularly variable The same authors also found variations in p of 1% for Nova Serpentis 1970, but no variations for Nova Vulpeculae No 1 1968 According to Zellner (1971), Mie theory suggests that the polarization of HR Del 1967 can be explained by scattering from grains of iron or graphite within an asymmetric circumstellar cloud, and de nitely not pure silicate Such non-volatile matter may be the condensation of material ejected at the outburst, or may be the debris remaining from a previous outburst event Zellner (1971) also commented on the infrared excesses seen in Novae Ser 1970 and Aquilae 1970, attributing them to thermal radiation from grains in the dust shell Noting that the strong infrared uxes did not appear during Epoch I for Nova Del, nor for Nova Ser, during the early stages when the variable polarization was seen, Zellner suggested two distinct generations of circumstellar grains It is perhaps possible that the high ejection velocities of the fast novae prevent the formation of small grains, at least in the initial stages, or the lack of intrinsic polarization may simply indicate no source dust in the system Zellner proposed that the small grains responsible for the production of the polarization are precursors of condensation nuclei for the accretion of much larger particles of radius 1 m For future fast novae, it is important to combine polarimetry with infrared photometry to follow the suggested grain developments Pirrola & Korhonen (1979) made observations of Nova Cygni 1978 and noted an increase in polarization from 16% to 19% over a period of a week The change correlated with infrared observations promotes a notion of there being a dust forming stage Combined with photometry which revealed short-term ickering in Nova Cygni 1978, Blitzstein, Bradstreet, Hrivnak, et al (1980) also reported on polarimetric measurements made in the early phase of the outburst, prior to the time of dust formation After consideration of the interstellar component, a residual intrinsic polarization of 023% was deduced, attributable to non-spherical scattering of H emission A rough estimate of the distance was obtained by considering the interstellar component Variable, and ence intrinsic polarization, was observed by Eggen, Mathewson & Serkowski (1967) for Nova Pyxidis in the very early stages of its outburst in 1966 1967 Little comment was made except that the lack of signi cant changes in the H line suggest that the polarization was generated in the outer shell of the nova Kemp & Rudy (1976) observed Nova Cygni 1975 over a wide range of wavelengths, including narrow-band studies of the H emission No structure in p ( ),.

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or ( ), was seen across this intense feature and the general form of p ( ) corresponded to the behaviour expected of Serkowski s Law It was concluded that the recorded polarization was clearly interstellar Intrinsic circular polarization, however, was detected with a Zeeman-like structure across the H emission The estimated eld in the emission region was 100 G If the system is interpreted as being a pair of dwarf stars, this implies an impossibly large eld, 1017 G, at the nucleus, say at the white dwarf surface The situation is reconcilable by considering the outburst to be highly asymmetrical, taking the form of conical and polar plumes such that geometry requires very high, but reasonable, elds on the surface of the central star This scenario was revealed more dramatically by Stockman, Schmidt & Lamb (1988) when the same nova had declined by late 1987 to magnitude 17 and relabelled as V 1500 Cygni Circular polarization was detected and interpreted as high harmonic optical cyclotron emission from an accreting, magnetic white dwarf primary They recorded a periodic variation of v at P D 0d 137154, with a semi-amplitude of 15%, corresponding to the rotation period of a star with a large dipolar eld The suggestion is that the pre-nova system was a synchronised AM Her magnetic variable During the outburst and subsequent dense wind phase, coupling between the white dwarf and expanded envelope produced the change in period rst noted by photometry Substantial polarization variation during minimum light at the eclipse stage of DQ Her was monitored by Dibai & Shakhovskoi (1967), thus allowing determination of the position for the orbital plane of the close binary system, this being very similar to the direction of the major axis of the envelope after the 1934 nova outburst Perhaps the most remarkable polarimetric discovery related to the same object displaying a remarkable 71-second light variation, is that of Swedlund, Kemp & Wolstencroft (1974) who found variable circular polarization with a period of 142 s, or twice that of the light period It was concluded that the object contains an oblique magnetic rotator The same research group (Kemp, Swedlund & Wolstencroft, 1974) also discovered a periodic linear polarization with the same period of 142 s, and offered a simple model The nova-like system V 3885 Sgr, sometimes referred to as Bond s star, was observed in 1983 by Metz (1989) to investigate the binary character of the system The standard deviations of the measurements were surprisingly in accordance with photon statistics, with no periodicity detectable Phase diagrams were constructed around various assumed values, but no periodic variation was signi cant, with the conclusion that the study of polarization does not help the understanding of this object Nova Cassiopeiae 1993, or V 705 Cas was monitored by Okazaki, Kurihara, Hirata, et al (1996) in its early stages and was found to display irregular variations of p on time scales of several days, and it was suggested that its intrinsic polarization in the early decline phase was caused by dust scattering The observations were modelled by Kawabata, Seki, Matsumuru et al (1996) who suggested that that the dust size distribution was quite narrow in the arly stages of the outburst, but became wider later.

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