Modern galaxy formation theory suggests that the misalignment between stellar and gaseous components usually results from an external gas accretion and/or interaction with other galaxies. The extreme case of the kinematic misalignment is demonstrated by so-called galaxies with counterrotation that possess two distinct components rotating in opposite directions with respect to each other. We provide an in-deep analysis of galaxies with counterrotation from IllustrisTNG100 cosmological simulations. We have found 25 galaxies with substantial stellar counterrotation in the stellar mass range of 2 × 109 − 3 × 1010 M⊙ . In our sample the stellar counterrotation is a result of an external gas infall happened ≈2 − 8 Gyr ago. The infall leads to the initial removal of pre-existing gas, which is captured and mixed together with the infalling component. The gas mixture ends up in the counterrotating gaseous disc. We show that $\approx 90\%$ of the stellar counterrotation formed in-situ, in the counterrotating gas. During the early phases of the infall, gas can be found in inclined extended and rather thin disc-like structures, and in some galaxies they are similar to (nearly-) polar disc or ring-like structures. We discuss a possible link between the gas infall, AGN activity and the formation of misaligned components. In particular, we suggest that the AGN activity does not cause the counterrotation, although it is efficiently triggered by the retrograde gas infall, and it correlates well with the misaligned component appearance. We also find evidence of the stellar disc heating visible as an increase of the vertical-to-radial velocity dispersion ratio above unity in both co- and counterrotating components, which implies the importance of the kinematical misalignment in shaping the velocity ellipsoids in disc galaxies.

A parallel implementation of the magneto-hydrodynamical code for global modeling of the galactic evolution is reported. The code is parallelized by using MPI interface, and it shows ideal scaling up to 200-300 cores on Lomonosov supercomputer with fast interconnect. In the benchmarking of this code, we study the dynamics of a magnetized gaseous disk of a galaxy with a bar. We run a high-resolution 3D magnetohydrodynamic simulation taking into account the Milky Way-like gravitational potential, gas self-gravity and a network of cooling and heating processes in the interstellar medium. By using this simulation the evolution of morphology and enhancement of the magnetic field are explored. In agreement to hydrodynamical models, when the bar is strong enough, the gas develops sharp shocks at the leading side of the bar. In such a picture we found that when typically the magnetic field strength traces the location of the largescale shocks along the bar major axis, the magnetic field pressure weakens the shocks and reduces the inflow of gas towards the galactic center.