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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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format to a new one This might mean that we would want to revisit the whole issue of file format Perhaps we would be better off with a format that would ot require conversion from one version of MovieCat to the next Second, we would have to modify the code for both the MovieItemView and MovieEditor classes to account for the new attributes However, the Swing GridBagLayout we've used lends itself to easily modifying component layout, and adding the new code would not be much more difficult than writing the original The fact that all the new attributes will be isolated in the Movie class will make the process easier What about adding searching capability This should be easy There are two approaches we could use In either case, the user interface would be most easily added to the MainView class First, we could add a search method to the MovieModel class, and then use it from the MainView interface A second approach would be to use the iterator provided by the MovieModel, and implement the search within MainView Keeping the search within the MovieModel would make the system less sensitive to future changes, but it would limit the searches to whatever the MovieModel class provides Building a search based on using the iterator would allow the most flexibility on which fields could be used for the search, but would be sensitive to changes Either way will easily be added to the current MovieCat code Some of the other changes, such as adding images or IMDb connectivity would require a significant effort to understand what image formats are available, or how to connect and use the IMDb The effort to add either could equal or exceed the original effort, but would still fit within the existing design The same seems true for the other features The isolation of the model from the GUI, and the use of MVC will make it easy to add features to MovieCat.

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Abramyan, GV (1981) Polarimetric investigations of red supergiants Soob Byurakan Obs, 52, 24 43 [ 313] Abramyan, GV (1982) The interstellar component of linear olarization of 12 red supergiants Soob Byurakan Obs, 53, 40 76 [313] Arsenijevi , J, Kubi ela, A, Vince, I (1980) c c Surprisingly high polarization of Cephei IBVS, No: 1859, Budapest [313] Clarke, D, Schwarz, HE (1984) The polarization of Orionis II Interpretation of narrow-band measures A&A, 132, 375 380 [314, 314] Coyne, (SJ) GV, Kruszewski, A (1968) Wavelength dependence of polarization XI Mu Cephei AJ, 73, 20 25 [313]. of Orionis II Interpretation of narrow-band measures . In VS .NET Using Barcode generation for .NET .Related:

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