A. V. Khoperskov

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. Comprehensive gravitational potential accounts for contributions from the stellar bulge, two and four armed spiral structure, stellar disk, dark halo and takes into account self-gravitation of the gaseous component. Gas clouds in our model form in the spiral arms due to shear and wiggle instabilities and turn into molecular clouds after

Early-type disk galaxies: Structure and kinematics

tsimgt 100

Global gravitationally organized spiral waves and the structure of NGC 5247

Myr. At the times

Gravitational Stability and Dynamical Overheating of Galactic Stellar Disks

tsim 100 - 300

Giant molecular cloud scaling relations: the role of the cloud definition

Myr the clouds form hierarchical structures and agglomerations with the sizes of 100 pc and greater. We analyze physical properties of the simulated clouds and find that synthetic statistical distributions like mass spectrum, mass-size relation and velocity dispersion are close to those observed in the Galaxy. The synthetic

Dynamics of Gaseous Disks in a Non-axisymmetric Dark Halo

l-v

Numerical code for multi-component galaxies: from N-body to chemistry and magnetic fields

(galactic longitude - radial velocity) diagram of the simulated molecular gas distribution resembles observed one and displays a structure with appearance similar to Molecular Ring of the Galaxy. Existence of this structure in our modelling can be explained by superposition of emission from the galactic bar and the spiral arms at

Interaction between collisionless galactic discs and non-axisymmetric dark matter haloes

sim

Interaction of the dark-matter cusp with the baryonic component in disk galaxies

3-4 kpc.

Structure and kinematics of polar ring galaxies: new observations and estimation of the dark halo shape

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 Observatory of the Russian Academy of Sciences aimed to study the structure and kinematic properties of early-type disk galaxies. The radial profiles of the stellar radial velocities and the velocity dispersion are measured. N-body simulations are used to construct dynamical models of galaxies containing a stellar disk, bulge, and halo. The masses of individual components are estimated formaximum-mass disk models. A comparison of models with estimated rotational velocities and the stellar velocity dispersion suggests that the stellar disks in lenticular galaxies are “overheated”; i.e., there is a significant excess velocity dispersion over the minimum level required to maintain the stability of the disk. This supports the hypothesis that the stellar disks of S0 galaxies were subject to strong gravitational perturbations. The relative thickness of the stellar disks in the S0 galaxies considered substantially exceed the typical disk thickness of spiral galaxies.