  Cataclysmic Variables (CVs) are close binary systems where mass is
transferred from a red dwarf star to a white dwarf star via an accretion disk.
The flickering is observed as stochastic variations in the emitted radiation
both in the continuum and in the emission line profiles. The main goal of our
simulations is to compare synthetic Doppler maps with observed ones, aiming to
constrain the flickering properties and wind parameters. A code was developed
which generates synthetic emission line profiles of a geometrically thin and
optically thick accretion disk. The simulation allows us to include flares in a
particular disk region. The emission line flares may be integrated over
arbitrary ``exposure'' times, producing the synthetic line profiles. Flickering
Doppler maps are created using such synthetic time series. The presence of a
wind inside the Roche lobe was also implemented. Radiative transfer effects in
the lines where taken into account in order to reproduce the single peaked line
profiles frequently seen in nova-like CVs.
