  The stochastic variability (flickering) of the nova-like system (subclass of
cataclysmic variable) MV Lyr yields a complicated power density spectrum with
four break frequencies. Scaringi et al. (2012) analysed high-cadence Kepler
data of MV Lyr, taken almost continuously over 600 days, giving the unique
opportunity to study multicomponent Power Density Spectra (PDS) over a wide
frequency range. We modelled this variability with our statistical model based
on disc angular momentum transport via discrete turbulent bodies with an
exponential distribution of the dimension scale. Two different models were
used, a full disc (developed from the white dwarf to the outer radius of ~10^10
cm) and a radially thin disc (a ring at a distance of ~10^10 cm from the white
dwarf) that imitates an outer disc rim. We succeed in explaining the two lowest
observed break frequencies assuming typical values for a disc radius of 0.5 and
0.9 times the primary Roche lobe and an alpha parameter of 0.1-0.4. The highest
observed break frequency was also modelled, but with a rather small accretion
disc with radius of 0.3 times the primary Roche lobe and a high alpha value of
0.9 consistent with previous findings by Scaringi (2014). Furthermore, the
simulated light curves exhibit the typical linear rms-flux proportionality
linear relation and the typical log-normal flux distribution. As the turbulent
process is generating fluctuations in mass accretion that propagate through the
disc, this confirms the general knowledge that the typical rms-flux relation is
mainly generated by these fluctuations. In general a higher rms is generated by
a larger amount of superposed flares which is compatible with a higher mass
accretion rate expressed by a larger flux.
