The Accretion Model of Dwarf Novae with Application To Z Chamaeleontis

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Abstract
The processes that arise as a result of mass transfer between the red and blue components in dwarf nova type binary systems are examined. It is shown that the outbursts themselves may be accounted for by unstable mass transfer by the red component. The consequent behaviour of the impact hot spot and of the accretion disc surrounding the blue component is shown in the steady state approximation to be in detailed agreement with the observed behaviour of the eclipsing system Z Cha, during both the quiescent normal state, and the outburst state. The cause of such a red component instability is considered together with effects due to time dependent evolution of accretion discs. Problems associated with a nuclear burning instability as an alternative explanation of dwarf nova outbursts are examined. In particular it is shown that the disc behaviour observed in Z Cha is difficult to achieve through such a mechanism. It is noted that many types of variable and unstable stars may involve similar processes to those discussed in this paper.

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