  We present the results of 3D-hydrodynamical simulations of accretion flow in
the eclipsing dwarf nova V1239 Her in quiescence. The model includes the
optical star filling its Roche lobe, a gas stream emanating from the inner
Lagrangian point of the binary system, and the accretion disc structure. A cold
hydrogen gas stream is initially emitted towards a point-like gravitational
centre. A stationary accretion disc is formed in about 15 orbital periods after
the beginning of accretion. The model takes into account partial ionization of
hydrogen and uses realistic cooling function for hydrogen. The light curve of
the system is calculated as the volume emission of optically thin layers along
the line of sight up to the optical depth \tau =2/3 calculated using
Planck-averaged opacities. The calculated eclipse light curves show good
agreement with observations, with the changing shape of pre-eclipse and
post-eclipse light curves being explained entirely due to ~ 50% variations in
the mass accretion rate through the gas stream.
