We photometrically observed the VY Scl-type cataclysmic variable KR Aurigae after its final rise from the fading episode in 2000–2001 .
Time-resolved observation revealed that the light curve is dominated by 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 a result of 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 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 q =0.43 ( MV Lyr ) and q =0.60 ( KR Aur ) .