Titlebook: Novae and Related Stars; Proceedings of an In M. Friedjung Conference proceedings 1977 D. Reidel Publishing Company, Dordrecht, Holland 197

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Cross Correlation Detection of Rapid Stellar Variability Using Two Telescopesandwidths B . 0.1 Hz may be expected of a variety of irregular variables including dwarf novae and X-ray binaries. Stochastic variability is harder to detect than periodic variability because its spectrum is likely to be a continuum, not necessarily distinguishable from the spectrum of the noise due

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The Binary Nature of the Nova-Like Variable CD -42° 14462ponent near one solar mass. The implied model is very similar to that found for the U Gem stars and old novae: an unseen lower main sequence star is transferring material onto a white dwarf. An accretion disk about the degenerate star is detected in weak H emissions. The phase dependence of both the

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Malleable

opportune

緯線

The Expansion of Novae before Light Maximum and the Formation of the Principal Envelopee in order to understand the mechanism which is responsible for the origin of the principal envelope we should analyse all the events which are observed from the moment of explosion of a Nova up to the moment of appearance of the principal spectrum of the star. At first we should mention that alread

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choroid

淘氣

Physical Parameters of Prenovae and Outburst Amplitudesitudes of novae at minimum light versus amplitude of the outburst. Three dwarf novae are found well separated from the novae, five recurrent novae mix with the high luminosity end of the nova sequence. Due to the small scatter in absolute magnitudes at maximum a noticeable dependence of outburst amp

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Mass Transfer and Accretion Disc Flow in Close Binary Systemscated. The interpretation of optical observations is expected to be further confused by a dominant part of the optical emission from the regions being due to reprocessed ultraviolet and soft X-ray flux originating close to the primary. In particular gas motion in the direction perpendicular to the o