Abstract
Cataclysmic binary systems consist of a white dwarf star, conventionally called the primary star, and a companion secondary star that is usually a cool main-sequence star (red dwarf) of late spectral type G, K or M. These variable binary star systems have orbital periods lying between 1 and 15 hours. The orbital period and ratio of the masses of the two stars are such that the secondary star fills its Roche lobe, causing gas to flow from the secondary toward the degenerate primary star. In the absence of a magnetic field, this gas forms an accretion disk around the primary star; the gas streams onto the magnetic poles when there is a strong magnetic field (Wade and Ward, 1985).
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