Large, highly organized radio structures near the galactic centre

Yusef‐Zadeh, F.; Morris, Mark; Chance, D.

doi:10.1038/310557a0

Cited by 362 publications

(266 citation statements)

References 26 publications

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“…Complicated structures, e.g., nonthermal filaments including Radio Arc, are observed in the Galactic center region, which probably attribute to magnetic fields (Yusef-Zadeh, Morris & Chance 1984;Tsuboi et al 1986;Chuss et al 2003;Nishiyama et al 2010;Morris 2014). Crocker et al (2010) gave a lower limit on the field strength, > 50 µG, over the central 400 pc region from a non-thermal radio spectrum.…”

Section: E-mail: Stakeru@nagoya-ujp (Tks)mentioning

confidence: 99%

Stochastic non-circular motion and outflows driven by magnetic activity in the Galactic bulge region

Suzuki

Fukui

Torii

et al. 2015

Mon. Not. R. Astron. Soc.

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By performing a global magneto-hydrodynamical simulation for the Milky Way with an axisymmetric gravitational potential, we propose that spatially dependent amplification of magnetic fields possibly explains the observed noncircular motion of the gas in the Galactic center region. The radial distribution of the rotation frequency in the bulge region is not monotonic in general. The amplification of the magnetic field is enhanced in regions with stronger differential rotation, because magnetorotational instability and field-line stretching are more effective. The strength of the amplified magnetic field reaches > ∼ 0.5 mG, and radial flows of the gas are excited by the inhomogeneous transport of angular momentum through turbulent magnetic field that is amplified in a spatially dependent manner. In addition, the magnetic pressuregradient force also drives radial flows in a similar manner. As a result, the simulated position-velocity diagram exhibits a time-dependent asymmetric parallelogram-shape owing to the intermittency of the magnetic turbulence; the present model provides a viable alternative to the bar-potential-driven model for the parallelogram-shape of the central molecular zone. This is a natural extension into the central few 100 pc of the magnetic activity, which is observed as molecular loops at radii from a few 100 pc to 1 kpc. Furthermore, the time-averaged net gas flow is directed outward, whereas the flows are highly time-dependent, which we discuss from a viewpoint of the outflow from the bulge.

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Section: E-mail: Stakeru@nagoya-ujp (Tks)mentioning

confidence: 99%

Stochastic non-circular motion and outflows driven by magnetic activity in the Galactic bulge region

Suzuki

Fukui

Torii

et al. 2015

Mon. Not. R. Astron. Soc.

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“…The most striking manifestation of the magnetic field in the diffuse ISM (or more precise: in the intercloud medium) are the Non-thermal Filaments (NTFs), evident in radio continuum images of the Galactic Center [44]. These structures -unique to the Galactic Center -are observed isolated or in bundles of parallel strands, they run (within 20-30 deg) orthogonal to the Galactic plane for a few tens of parsecs, while their transverse dimension is only a fraction of a parsec.…”

Section: Magnetic Fields In the Diffuse Gc Ismmentioning

confidence: 99%

Galactic Center Molecular Clouds

Güsten

Philipp

1997

Springer Proceedings in Physics

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At a distance of 8 kpc only, the center of the Galaxy provides a unique testbed for studies about the physics of the interstellar medium and star formation in the nuclei of galaxies. Since it shares many properties of other, more spectacular nuclei, a detailed investigation of the Galactic Center is a necessary step to gain better understanding of the physical processes governing galactic nuclei in general. We review the characteristics of the central molecular cloud layer, the physical properties of these clouds, and their interplay with the magnetic field.Comment: 10 pages, 3 figures. Version with full graphics available from ftp://ftp.mpifr-bonn.mpg.de/outgoing/sphilipp (Co)authored by members of the MPIfR (Sub)millimeter Astronomy Group. To appear in the Proceedings of the 4th Cologne-Bonn-Zermatt-Symposium "The Dense Interstellar Medium in Galaxies" eds. S. Pfalzner, C. Kramer, C. Straubmeier, & A. Heithausen (Springer: Berlin

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“…Yusef-Zadeh et al 1984, Lang et al 1999, Yusef-Zadeh et al 2004, LaRosa et al 2004) have been detected within 1 • from the Galactic center. They are almost perpendicular to the Galactic plane, although some of the newly found filaments are not (LaRosa et al 2004).…”

Section: Magnetic Fields In the Galactic Central Regionmentioning

confidence: 97%

Magnetic fields in our Milky Way Galaxy and nearby galaxies

Han

2012

Proc. IAU

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Abstract. Magnetic fields in our Galaxy and nearby galaxies have been revealed by starlight polarization, polarized emission from dust grains and clouds at millimeter and submillimeter wavelength, the Zeeman effect of spectral lines or maser lines from clouds or clumps, diffuse radio synchrotron emission from relativistic electrons in interstellar magnetic fields, and the Faraday rotation of background radio sources as well as pulsars for our Milky Way. It is easy to get a global structure for magnetic fields in nearby galaxies, while we have observed many details of magnetic fields in our Milky Way, especially by using pulsar rotation measure data. In general, magnetic fields in spiral galaxies probably have a large-scale structure. The fields follow the spiral arms with or without the field direction reversals. In the halo of spiral galaxies magnetic fields exist and probably also have a large-scale structure as toroidal and poloidal fields, but seem to be slightly weaker than those in the disk. In the central region of some galaxies, poloidal fields have been detected as vertical components. Magnetic field directions in galaxies seem to have been preserved during cloud formation and star formation, from large-scale diffuse interstellar medium to molecular clouds and then to the cloud cores in star formation regions or clumps for the maser spots. Magnetic fields in galaxies are passive to dynamics.

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Large, highly organized radio structures near the galactic centre

Cited by 362 publications

References 26 publications

Stochastic non-circular motion and outflows driven by magnetic activity in the Galactic bulge region

Stochastic non-circular motion and outflows driven by magnetic activity in the Galactic bulge region

Galactic Center Molecular Clouds

Magnetic fields in our Milky Way Galaxy and nearby galaxies

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