Superhumps in V348 Pup

The eclipsing nova-like cataclysmic variable star V348 Pup exhibits a persi stent luminosity modulation with a period 6 per cent longer than its 2.44-h orbital period (P-orb) This has been interpreted as a 'positive superhump' resulting from a slowly precessing non-axisymmetric accretion disc gravita tionally interacting with the secondary. We find a clear modulation of mid- eclipse times on the superhump period, which agrees well with the predictio ns of a simple precessing eccentric disc model. Our modelling shows that th e disc light centre is on the far side of the disc from the donor star when the superhump reaches maximum light. This phasing suggests a link between superhumps in V348 Pup and late superhumps in SU UMa systems. Modelling of the full light curve and maximum entropy eclipse mapping both show that the disc emission is concentrated closer to the white dwarf at superhump maxim um than at superhump minimum. We detect additional signals consistent with the beat periods between the implied disc precession period and both 1/2 P- orb and 1/3 P-orb.