  Circumstellar disks in binaries are perturbed by the companion gravity
causing significant alterations of the disk morphology. Spiral waves due to the
companion tidal force also develop in the vertical direction and affect the
disk temperature profile. These effects may significantly influence the process
of planet formation. We perform 3D numerical simulations of disks in binaries
with different initial dynamical configurations and physical parameters. Our
goal is to investigate their evolution and their propensity to grow planets. We
use an improved version of the SPH code VINE modified to better account for
momentum and energy conservation. The energy equation includes a flux--limited
radiative transfer algorithm and the disk cooling is obtained via "boundary
particles". We model a system made of star/disk + star/disk where the secondary
star (and relative disk) is less massive than the primary. The numerical
simulations performed for different values of binary separation and disk
density show that the disk morphology is substantially affected by the
companion perturbations. Trailing spiral shock waves develop when the stars
approach their pericenter. Strong hydraulic jumps occur at the shock front
creating breaking waves and a consistent mass stream between the two disks,
significantly heating them. The high gas temperature may prevent the ice
condensation by moving outward the "snow line". The hydraulic jumps may slow
down or even halt the dust coagulation process. At apocenter these
perturbations are reduced and the disks are cooled down and less eccentric. The
strength of the hydraulic jumps, disk heating, and mass exchange depends on the
binary separation, and for larger semi-major axes, the tidal spiral pattern is
substantially reduced.
