Optical and IR light curves of VV Puppis

We present optical (0.36–0.6 μm) light curves with time resolutions of seconds and infrared (IR) (1.25–2.2 μm) light curves with time resolutions of minutes for VV Puppis during a high state. The optical light curves show a single hump with largest amplitude in the V filter, while the IR light curves show a double hump sinusoidal variation. Flickering is evident in both the optical and IR light curves, with the largest amplitude in optical B light. Through subtraction of the low state fluxes from our high state values, we obtain a flux distribution of the accretion column which peaks at 0.55 μm and becomes $$\nu^2$$ in the IR, consistent with current cyclotron models. Comparison of the observed IR variations throughout the orbit with the expected variations due to an M4 star heated by an accretion column at an inclination of 66° suggests that the IR light is a combination of the secondary star plus contributions from two emitting poles.