Аннотация:Numerical simulations of thick galactic disks, are described, and the results are compared with the available observational data. The disks comprise 200 interacting mass-points embedded in a halo gravitational field of relative mass M(h)/M(d)=0, 1, 2, and 3, respectively. At the beginning of the simulations, the disks had an exponential density distribution within the radius R; at the end of the simulation, the velocity dispersions c(z), c(r), and the c(z)/c(r) ratio diminished with radial distance r. In models with M(h)/M(d) greater than or equal to 1, the disk half-thickness Delta was independent of r, as observed. It is found that although Delta increase when M(h) becomes smaller, it remains smaller than M(h) even in the case M(h)=0. Comparison of model estimates with the observed ratio Delta/L (L being the disk scale factor) showed that the models having M(d)/M(h) less than or equal to 2 are closely fitted by spiral galaxies. In massive halo systems, the layer of diffuse matter may be as thick as the stellar disk.