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The stochastic variability (flickering) of the nova-like system (subclass ofcataclysmic variable) MV Lyr yields a complicated power density spectrum withfour break frequencies. Scaringi et al. (2012) analysed high-cadence Keplerdata of MV Lyr, taken almost continuously over 600 days, giving the uniqueopportunity to study multicomponent Power Density Spectra (PDS) over a widefrequency range. We modelled this variability with our statistical model basedon disc angular momentum transport via discrete turbulent bodies with anexponential distribution of the dimension scale. Two different models wereused, a full disc (developed from the white dwarf to the outer radius of ~10^10cm) and a radially thin disc (a ring at a distance of ~10^10 cm from the whitedwarf) that imitates an outer disc rim. We succeed in explaining the two lowestobserved break frequencies assuming typical values for a disc radius of 0.5 and0.9 times the primary Roche lobe and an alpha parameter of 0.1-0.4. The highestobserved break frequency was also modelled, but with a rather small accretiondisc with radius of 0.3 times the primary Roche lobe and a high alpha value of0.9 consistent with previous findings by Scaringi (2014). Furthermore, thesimulated light curves exhibit the typical linear rms-flux proportionalitylinear relation and the typical log-normal flux distribution. As the turbulentprocess is generating fluctuations in mass accretion that propagate through thedisc, this confirms the general knowledge that the typical rms-flux relation ismainly generated by these fluctuations. In general a higher rms is generated bya larger amount of superposed flares which is compatible with a higher massaccretion rate expressed by a larger flux.

Rms-flux relation and fast optical variability simulations of the nova-like system MV Lyr