EMISSION-LINE VARIATIONS OF THE NOVA-LIKE VARIABLE PX ANDROMEDAE (=PG-0027+260)

We present time-resolved spectroscopy of the nova-like variable PX And in both high and low accretion states. In common with many other nova -like objects, it displays single-peaked emission lines incompatible w ith an accretion disc origin. Continuum emission displays a shallow ec lipse but high-excitation line emission remains uneclipsed, suggesting an origin close to the white dwarf. Balmer and HeI lines undergo core absorption at times centred on orbital phase 0.5, and contain maximum flux at phase 0.8. We show that the high-excitation emission shares a common velocity with the white dwarf, but we cannot predict the low-e xcitation line distributions without an accurate position-velocity rel ation. We discuss some likely models for this system and constrain the height above the disc at which emission must originate to remain unec lipsed.