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High-speed white light photometry of the cataclysmic variable star Z Cha is used to study the structure of the system and to derive the properties of its components. The white dwarf and bright spot eclipse timings require a mass ratio, |q=M_ R/M ₖ₃| of |0. 146 q0. 153| with corresponding inclinations of 81°. 9>i>>81°. 6. The infalling stream passes through the light centre of the bright spot. If the central luminous object is the white dwarf its mass is 0. 54±0. 01 |M_| which corresponds to a secondary star mass of 0. 081±0. 003 |M_|. Agreement between colour and brightness temperatures for the white dwarf and bright spot provide a rough confirmation of the 97 pc distance.
Wood et al. (Tue,) studied this question.