The structure of matter flows in semi-detached binaries after the termination of mass transfer

We present the results of three-dimensional gas-dynamical simulations of ma tter flows in semidetached binaries after termination of the mass transfer between the components of the system. The structure of the residual accreti on disk is studied. When the mass transfer has ended, the quasi-elliptical disk becomes circular and its structure changes: tidal interactions result in the formation of a second arm in the spiral shock wave. In addition, a c ondensation (blob) moving through the disk with variable velocity is formed . The blob is maintained by interactions with the arms of the spiral shock and exists essentially over the entire lifetime of the disk. We also show t hat, for a viscosity corresponding to alpha similar to 0.01 (typical for ob served accretion disks), the lifetime of the residual disk is about 50 orbi tal periods. (C) 2001 MAN "Nauka/Interperiodica".