Stochastic models of the vertical structure of turbulent gaseous disks of galaxies

On the basis of stochastic methods, a numerical simulation of the quasiequilibrium turbulent gas disk of a galaxy located in thermal and dynamic equilibrium in the field of gravity of the stellar disk is carried out. The cumulative effect on the interstellar medium (ISM) of the physical mechanisms responsible for the generation of turbulence was modeled using the spectral version of forcing, that is, by creating perturbations of the velocity field with given spectral characteristics. The influence of velocity field perturbations on the dynamics of interstellar gas was investigated in the framework of numerical experiments with different input parameters, in particular, depending on the spatial scales and pump intensity. It is established that using this approach provokes the formation of a quasi-stable vertical structure in the gas disk, which is conformed qualitatively and quantitatively with observations of ISM in the disks of spiral galaxies.