Flickering of accreting white dwarfs: the remarkable amplitude–flux relation and disc viscosity

We analyse 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 1029 to 1033 erg s−1 Å−1, as a ‘statistically perfect correlation with correlation coefficient 0.96 and p-value ∼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 nine accreting white dwarfs with ΔF = 0.36(±0.05)F av, σrms = 0.086(±0.011)F av, and σrms/ΔF = 0.24 ± 0.02. Overall, our results indicate that the viscosity in the accretion discs is practically the same for all nine objects in our sample, in the mass accretion rate range 2 × 10−11 − 2 × 10−7 M⊙ yr−1.