3D MHD Modeling of the Gaseous Structure of the Galaxy.

  title={3D MHD Modeling of the Gaseous Structure of the Galaxy.},
  author={G. Gomez and Donald P. Cox},
We show the results of our 3D MHD simulations of the o w of the Galactic atmosphere as it responds to a spiral perturbation in the potential. 
Recent observations of gaps and non-axisymmetric features in the dust distributions of transition disks have been interpreted as evidence of embedded massive protoplanets. However, comparing the
Turbulence in the interstellar medium
Turbulence is ubiquitous in the insterstellar medium and plays a major role in several processes such as the formation of dense structures and stars, the stability of molecular clouds, the
Kinematics of Spiral-Arm Streaming in M51
We use CO and Hα velocity fields to study the gas kinematics in the spiral arms and interarms of M51 (NGC 5194), and fit the 2D velocity field to estimate the radial and tangential velocity
Multi-Wavelength Observations and Modeling of Loop I
The article aims to overview the origin and current dynamical state of a giant structure on the northern galactic sky—the radio Loop I extending from ≈ − 45 ∘ to ≈ + 45 ∘ in longitudes and up to ≈ 80
Giant cometary H iiregions and molecular bow shocks in spiral arms of galaxies: M 83
  • Y. Sofue
  • Physics
    Publications of the Astronomical Society of Japan
  • 2018
A number of giant cometary HII regions (GCH) sheathed inside molecular bow shocks (MBS) are found along spiral arms of the barred galaxy M83. The open cone structure is explained by a model of
FOREST Unbiased Galactic Plane Imaging Survey with the Nobeyama 45 m telescope (FUGIN). IV. Galactic shock wave and molecular bow shock in the 4 kpc arm of the Galaxy
The FUGIN CO survey revealed the three-dimensional structure of a galactic shock wave in the tangential direction of the 4 kpc molecular arm. The shock front is located at G30.5+00.0 + 95 km s−1 on
MHD simulations of ram pressure stripping of a disc galaxy
The removal of the interstellar medium (ISM) of disk galaxies through ram pressure stripping (RPS) has been extensively studied in numerous simulations. Nevertheless, the role of magnetic fields (MF)
Global enhancement and structure formation of the magnetic field in spiral galaxies
We study numerically large-scale magnetic field evolution and its enhancement in gaseous disks of spiral galaxies. We consider a set of models with the various spiral pattern parameters and the
On Shocks Driven by High-mass Planets in Radiatively Inefficient Disks. III. Observational Signatures in Thermal Emission and Scattered Light
Recent observations of the protoplanetary disk around the Herbig Be star HD 100546 show two bright features in infrared (H and bands) at about 50 au,with one so far unexplained. We explore the
Young and turbulent: the early life of massive galaxy progenitors
We present results from the ‘Ponos’ simulation suite on the early evolution of a massive, M_vir(z = 0) = 1.2 × 10^13 M_⊙ galaxy. At z ≳ 6, before feedback from a central supermassive black hole


Vertical extensions of galactic spiral arms
The vertical structure of the large scale galactic shock along spiral arms is studied, in order to understand the extended features or the ''wings'' of spiral arms observed by Kepner and recently
Hydrostatic equilibrium of gas, extent of cosmic ray confinement, and radio emission in the Galaxy
A detailed study of the hydrostatic equilibrium of the gas-field system perpendicular to the galactic plane in the neighborhood of the Sun, assuming that the magnetic field is parallel to the plane,
Magnetohydrodynamic Modeling of a Galactic Spiral Arm as a Combination Shock and Hydraulic Jump
We consider the interarm-to-arm transition for gas flow in the Galactic disk, modeled as a thick, magnetized, cloudless layer of gas in hydrostatic equilibrium with external gravity from stars, and
Large-Scale Shock Formation in Spiral Galaxies and its Implications on Star Formation
Two armed spiral galactic shock waves as triggering mechanism for gravitational collapse leading to star formation, considering gaseous disk motion using Schmidt model
The column density and scale height of free electrons in the galactic disk
The recent discoveries of millisecond pulsars in globular clusters located far from the Galactic plane provide the first direct measurements of the total extent and column density of diffuse ionized
Forbidden velocity gas detected in ultraviolet interstellar absorption toward four distant inner galaxy stars
We analyze International Ultraviolet Explorer high-dispersion observations of interstellar absorption toward HD 167402, HD 168941, HD 172140, and HD 173502, four distant, inner Galaxy, lower
Galactic hydrostatic equilibrium with magnetic tension and cosmic-ray diffusion
Three gravitational potentials differing in the content of dark matter in the Galactic plane are used to study the structure of the z-distribution of mass and pressure in the solar neighborhood. A
The gaseous galactic halo as inferred from the line spectra of the galaxies Markarian 509 and Fairall 9
Narrow interstellar absorption lines of S II 1259.52, Si II 1260.42, and Fe II 1608.46 due to gas in the disk and the halo of the Galaxy have been detected in the spectrum of the Seyfert galaxy Mrk
NGC 1058 - Gas motions in an extended, quiescent spiral disk
The motion of gas in the galaxy NGC 1058 is examined, using VLA observations to map emission in the 21-cm line. The hypothesis that the rotation curve drops faster than Keplerian at the outer edge of