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A thickening at the outer edge of the accretion disk is usually invoked toexplain the dips in the light curves of cataclysmic variables with stationarydisks at phases ~0.7. The non-collisional interaction between the stream andthe disk in the stationary solution raises the question of why matter appearsat a considerable height above the accretion disk in such systems. Ourthree-dimensional numerical modeling demonstrates that a thickening of the haloabove the disk can appear even in the absence of a direct collision between thestream and the disk. In the gas-dynamical flow pattern described with the"hot-line" model, a considerable fraction of the matter is accelerated in thevertical direction during the flow's interaction with the circumdisk halo. Thevertical motion of the gas due to the presence of the z component of thevelocity leads to a gradual thickening of the circumdisk halo. The computationsreveal the strongest thickening of the halo above the outer edge of the disk atphases ~0.7, in agreement with observations for stationary-disk cataclysmicvariables. This supports the hot-line model suggested earlier as a descriptionof the pattern of the matter flows in semi-detached binaries, and presents newpossibilities for interpreting the light curves of such systems.Comment: 12 pages, 10 figure

The possible nature of dips in the light curves of semidetached binaries with stationary disks