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Flickering is a universal phenomenon in accreting astronomical systems whichstill defies detailed physical understanding. It is particularly evident incataclysmic variables (CVs). Attempting to define boundary conditions formodels, the strength of the flickering is measured in several thousand lightcurves of more than 100 CVs. The flickering amplitude is parameterized by theFWHM of a Gaussian fit to the magnitude distribution of data points in a lightcurve. This quantity requires several corrections before a comparison betweendifferent sources can be made. While no correlations of the flickering strengthwith simple parameters such as component masses, orbital inclination or periodwere detected, a dependence on the absolute magnitude of the primary componentand on the CV subtype is found. In particular, flickering in VY Scl tpyenovalike variables is systematically stronger than in UX UMa type novalikes.The broadband spectrum of the flickering light source can be fit by simplemodels but shows excess in the $U$ band. When the data permitted to investigatethe flickering strength as a function of orbital phase in eclipsing CVs, such adependence was found, but it is different for different systems. Surprisingly,there are also indications for variations of the flickering strength with thesuperhump phase in novalike variables with permanent superhumps. In dwarfnovae, the flickering amplitude is high during quiescence, drops quickly at anintermediate magnitude when the system enters into (or returns from) anoutburst and, on average, remains constant above a given brightness threshold.

A comparative study of the strength of flickering in cataclysmic variables