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• W207921549 abstract "Q. J! R. astr. Soc. (1978) 19, 430-441 Novae versus Dwarf Novae: Energy Sources and Systematics A.D.Mallama Astronomy Program, University of Maryland, College Park, Maryland 20742, USA and Goddard Space Flight Center, Greenbelt, Maryland 20771, USA V.L.Trimble Department of Physics, University of California, Irvine, California 92717, USA and Astronomy Program, University of Maryland, College Park, Maryland 20742, USA (Received 1978 May 2) SUMMARY We review observational and theoretical work on classical novae and dwarf novae (U Gem, SS Cyg and Z Cam stars) that bears on the question of why binary systems with very similar component stars and orbits should have such different outburst behaviour. We are able to put together a consistent picture only for certain theories of the outbursts. In this picture, mass transfer occurs continuously at a steady rate from the late-type star towards the degenerate dwarf for all types of cataclysmic systems, most rapidly in the recurrent novae, somewhat slower in the classical novae and most slowly in the dwarf novae. The gas flows into an accretion disk in all cases. For the rapid transfer rates, the disk is always dense enough that viscosity is adequate to transfer angular momentum outwards and allow gas to accrete continuously on to the degenerate dwarf, where it accumulates until it is hot enough and dense enough to undergo nuclear reactions. Gravitational potential energy released during this accretion is the main energy source for classical novae at minimum light, while the mass-losing star (a giant) also contributes appreciably to minimum light in the recurrent novae. For the slowest mass transfer rates, gas accumulates for some time in the outer parts of the disk until a critical density is reached, viscosity increases and accretion occurs rapidly, liberating the available gravitational potential energy. Thus, in the dwarf novae, the main minimum light energy source is the impact of the gas stream from the late—type star hitting the accumulating disk, while the outbursts are caused by the sudden onset of accretion at the rate which is normal for classical novae at minimum light. Some or all of the transferred gas probably stays on the degenerate dwarf, so that an astronomer who waits patiently (about 10‘ yr for a typical system) can expect to see classical nova outbursts from at least some dwarf nova systems. CHARACTERISTICS OF THE OUTBURSTS AND SYSTEMS The eruptive or cataclysmic variable stars can be divided into four groups on the basis of their observed outburst behaviour. The four groups are the classical novae (Ne), recurrent novae (RNe), dwarf novae (DNe, with two subgroups, named for prototype stars Z Cam and U Gem, or, sometimes, SS Cyg) and nova-like variables (NL). Recent reviews of one or more of the groups are to be found in Robinson (1976), Warner (I 976), Friedjung (1977) and Gallagher & Starrfield (I978). 430 © Royal Astronomical Society 0 Provided by the NASA Astrophysics Data System" @default.
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• W207921549 date "1978-01-01" @default.
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• W207921549 title "NOVAE VERSUS DWARF NOVAE - ENERGY-SOURCES AND SYSTEMATICS" @default.
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