AN ACCRETION MODEL FOR THE ECLIPSING CATACLYSMIC VARIABLE PG-0859+415

The emission lines found in the majority of cataclysmic variables are generally used as tracers of accretion flows which dominate the light at optical wavelengths. It has been suggested from previous observatio ns that the eclipsing nova-like variable PG 0859 + 415 shows individua listic orbital characteristics that are inconsistent with canonical mo dels of stellar accretion. We present spectrophotometry of this star w hich suggests that the standard picture is not in conflict with observ ations. We provide evidence that the shallow optical eclipses are of a n extended bright spot rather than of the accretion disc, and that the low-excitation lines are dominated by a transient absorption componen t, perhaps a result of the bright spot or the accretion stream eclipsi ng the disc. We argue that this object may be another nova-like variab le displaying long-term or cyclic variations in mass transfer rate fro m the secondary star.