Optical (0.36-0.6 micron) light curves with time resolutions of seconds, and infrared (IR) (1.25-2.2 microns) light curves with time resolutions of minutes, are presented 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, a flux distribution of the accretion column is obtained which peaks at 0.55 micron and becomes v-squared 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 deg suggests that the IR light is a combination of the secondary star plus contributions from two emitting poles.
|Journal||Monthly Notices of the Royal Astronomical Society|
|Publication status||Published - 1983|