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Minimum velocity dispersion in stable stellar disks. Numerical simulations
N-body dynamical simulations are used to analyze the conditions for the gravitational stability of a three-dimensional stellar disk in the gravitational field of two rigid spherical components—a
Smoothed-Particle Hydrodynamics Models: Implementation Features on GPUs
The implementation is based on hierarchical grid sorting method using a cascading algorithm for parallel computations of partial sums at CUDA block and the parallelization efficiency of the algorithm for various GPUs of the Nvidia Tesla line is studied in the framework of galactic’ gaseous halos collisions models by the SPH-method.
Early-type disk galaxies: Structure and kinematics
Spectroscopic observations of three lenticular (S0) galaxies (NGC 1167, NGC 4150, and NGC 6340) and one SBa galaxy (NGC 2273) have been taken with the 6-m telescope of the Special Astrophysical
The Numerical Simulation of Shallow Water: Estimation of the Roughness Coefficient on the Flood Stage
The results of the numerical simulations of the dynamics of shallow waters for Volga-Akhtuba Floodplain are discussed. The mathematical model is based on the system of Saint-Venant equations.
Stellar velocity dispersion and mass estimation for galactic disks
Available velocity dispersion estimates for the old stellar population of galactic disks at galactocentric distances r⋍2L (where L is the photometric radial scale length of the disk) are used to
Kinematics and stellar disk modeling of lenticular galaxies
We present the results of spectroscopic observations of three S0-Sa galaxies: NGC 338, NGC 3245, and NGC 5440 at the SAO RAS 6-m BTA telescope. The radial distributions of the line-ofsight velocities
The simulation of molecular clouds formation in the Milky Way
Using 3D hydrodynamic calculations we simulate formation of molecular clouds in the Galaxy. The simulations take into account molecular hydrogen chemical kinetics, cooling and heating processes.
Global gravitationally organized spiral waves and the structure of NGC 5247
Using observational data, we build numerical N-body, hydrodynamical and combined equilibrium models for the spiral galaxy NGC 5247. The models turn out to be unstable as regards spiral structure
A dynamical model of the Galaxy
A series of dynamical models of the Galaxy is constructed assuming that the entire disk is near the gravitational-stability limit. This imposes constraints on the dynamical and kinematic parameters
The dynamics of linear perturbations in a differen- tially rotating accretion disk with a non-homogeneous vertical structure is investigated. We find that turbulent viscosity results in instability