The simulation of molecular clouds formation in the Milky Way

@article{Khoperskov2013TheSO,
  title={The simulation of molecular clouds formation in the Milky Way},
  author={Sergey Khoperskov and Evgenii O. Vasiliev and Andrey M. Sobolev and Alexander V. Khoperskov},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2013},
  volume={428},
  pages={2311-2320}
}
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… 

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References

SHOWING 1-10 OF 86 REFERENCES
The formation of molecular clouds in spiral galaxies
ABSTRACT We present Smoothed Particle Hydrodynamics (SPH) simulations of molecular cloudformation in spiral galaxies. These simulations model the response of a non-self-gravitating gaseous disk to a
Molecular Cloud Formation behind Shock Waves
Motivated by our previous paper, in which we argued for the formation of molecular clouds from large-scale flows in the diffuse Galactic interstellar medium, we examine the formation of molecular gas
Gas flow models in the Milky Way embedded bars
Context. The gas distribution and dynamics in the inner Galaxy present many unknowns, such as the origin of the asymmetry of the lu-diagram of the Central Molecular Zone (CMZ). On the other hand,
STAR FORMATION IN DISK GALAXIES. I. FORMATION AND EVOLUTION OF GIANT MOLECULAR CLOUDS VIA GRAVITATIONAL INSTABILITY AND CLOUD COLLISIONS
We investigate the formation and evolution of giant molecular clouds (GMCs) in a Milky-Way-like disk galaxy with a flat rotation curve. We perform a series of three-dimensional adaptive mesh
Spiral shocks and the formation of molecular clouds in a two-phase medium
We extend recent numerical results on molecular cloud formation in spiral galaxies by including a multiphase medium. The addition of a hot phase of gas enhances the structure in the cold gas, and
The Three-dimensional Structure of a Massive Gas Disk in the Galactic Central Region
Using high-resolution, three-dimensional hydrodynamical simulations, we investigate the structure of the interstellar medium (ISM) in the central 100 pc region in galaxies, taking into account the
A cloud/particle model of the interstellar medium - Galactic spiral structure
A cloud/particle model for gas flow in galaxies is developed. Instead of assuming that the interstellar medium is a continuum of gas governed by an equation of state, our model views it as a discrete
The Spatial and Mass Distributions of Molecular Clouds and Spiral Structures
The growth of molecular clouds resulting from cloud-cloud collisions and coalescence in the Galactic ring between 4 and 8 kpc are modeled, taking into account the presence of a spiral potential and
Gas dynamics and large-scale morphology of the Milky Way galaxy
We present a new model for the gas dynamics in the galactic disc inside the orbit of the Sun. Quasi-equilibrium flow solutions are determined in the gravitational potential of the deprojected COBE
RE-EXAMINING LARSON'S SCALING RELATIONSHIPS IN GALACTIC MOLECULAR CLOUDS
The properties of Galactic molecular clouds tabulated by Solomon et al. (SRBY) are re-examined using the Boston University-FCRAO Galactic Ring Survey of 13CO J = 1–0 emission. These new data provide
...
...