  H{\alpha} emission V/R variations caused by a discontinous mass transfer in
interacting binaries with a rapidly rotating accreting star are modelled
qualititatively for the first time. The program ZEUS-MP was used for a
non-linear 3-D hydrodynamical modeling of a development of a blob of gaseous
material injected into an orbit around a star. It resulted in the formation of
an elongated disk with a slow prograde revolution. The LTE radiative transfer
program SHELLSPEC was used to calculate the H{\alpha} profiles originating in
the disk for several phases of its revolution. The profiles have the form of a
double emission and exhibit V/R and radial velocity variations. However, these
variations should be a temporal phenomenon since imposing a viscosity in given
model would lead to a circularization of the disk and fading-out of given
variations.
