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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 rains 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 hence 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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