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We analyze heating and cooling processes in accretion disks in binaries. Forrealistic parameters of the accretion disks in close binaries (with accretionrates from 1e-12 to 1e-7 Msun/year and \alpha from 0.1 to 0.01), the gastemperature in the outer parts of the disk is from 1e4 to 1e6 K. Our previousgas-dynamical studies of mass transfer in close binaries indicate that, for hotdisks (with temperatures for the outer parts of the disk of several hundredthousand K), the interaction between the stream from the inner Lagrange pointand the disk is shockless. To study the morphology of the interaction betweenthe stream and a cool accretion disk, we carried out three-dimensional modelingof the flow structure in a binary for the case when the gas temperature in theouter parts of the forming disk does not exceed 13600 K. The flow patternindicates that the interaction is again shockless. The computations provideevidence that, as is the case for hot disks, the zone of enhanced energyrelease (the "hot line") is located beyond the disk, and originates due to theinteraction between the circum-disk halo and the stream.

Morphology of the Interaction Between the Stream and Cool Accretion Disk in a Semi-detached Binary Systems