  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).
