  We perform numerical simulations to investigate the stellar wind from
interacting binary stars. Our aim is to find analytical formulae describing the
outflow structure. In each binary system the more massive star is in the
asymptotic giant branch and its wind is driven by a combination of pulsations
in the stellar surface layers and radiation pressure on dust, while the less
massive star is in the main sequence. Time averages of density and outflow
velocity of the stellar wind are calculated and plotted as profiles against
distance from the centre of mass and colatitude angle. We find that mass is
lost mainly through the outer Lagrangian point L2. The resultant outflow
develops into a spiral at low distances from the binary. The outflowing spiral
is quickly smoothed out by shocks and becomes an excretion disk at larger
distances. This leads to the formation of an outflow structure with an
equatorial density excess, which is greater in binaries with smaller orbital
separation. The pole-to-equator density ratio reaches a maximum value of
$\sim10^5$ at Roche-Lobe Overflow state. We also find that the gas stream
leaving L2 does not form a circumbinary ring for stellar mass ratios above
0.78, when radiation pressure on dust is taken into account. Analytical
formulae are obtained by curve fitting the 2-dimensional, azimuthally averaged
density and outflow velocity profiles. The formulae can be used in future
studies to setup the initial outflow structure in hydrodynamic simulations of
common-envelope evolution and formation of planetary nebulae.
