  We analyze optical photometric data of short term variability (flickering) of
accreting white dwarfs in cataclysmic variables (KR Aur, MV Lyr, V794 Aql, TT
Ari, V425 Cas), recurrent novae (RS Oph and T CrB) and jet-ejecting symbiotic
stars (CH Cyg and MWC 560). We find that the amplitude-flux relationship is
visible over four orders of magnitude, in the range of fluxes from $10^{29}$ to
$10^{33}$ erg s$^{-1}$ \AA$^{-1}$, as a "statistically perfect" correlation
with correlation coefficient 0.96 and p-value $ \sim 10^{-28}$. In the above
range, the amplitude of variability for any of our 9 objects is proportional to
the flux level with (almost) one and the same factor of proportionality for all
9 accreting white dwarfs with $\Delta F = 0.36 (\pm 0.05) F_{av}$,
$\sigma_{rms} = 0.086(\pm 0.011) F_{av}$, and $\sigma_{rms} / \Delta F = 0.24
\pm 0.02$. Over all, our results indicate that the viscosity in the accretion
discs is practically the same for all 9 objects in our sample, in the mass
accretion rate range $2 \times 10^{-11} - 2\times10^{-7}$ $M_\odot$ yr$^{-1}$.
