Abstract
Abstract We photometrically observed the VY Scl-type cataclysmic variable KR Aurigae after its final rise from a fading episode in 2000–2001. A time-resolved observation revealed that the light curve is dominated by a persistent short-term variation with time-scales of minutes to tens of minutes. On some nights, quasi-periodic variations with periods of 10–15 min were observed. No coherent variation was detected. The power spectral density of the variation has a power-law component ($f^{-1.63}$). The temporal properties of the short-term variations in KR Aur present additional support for the possibility that flickering in CVs may be better understood as the result of a self-organized critical state, as in black-hole candidates. The light curve lacks “superhump”-type signals, which are relatively frequently seen in VY Scl-type systems and which are suggested to arise from a tidal instability of the accretion disk induced by changing mass-transfer rates. The present observation suggests a borderline of superhump excitation in VY Scl-type stars between mass ratios of $q = 0.43$ (MV Lyr) and $q = 0.60$ (KR Aur).
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