scholarly journals Sturm und Drang: The turbulent, magnetic tempest in the Galactic center

2013 ◽  
Vol 9 (S303) ◽  
pp. 395-398
Author(s):  
Brian C. Lacki
Keyword(s):  
Magnetic Fields ◽  
Galactic Halo ◽  
Galactic Center ◽  
Termination Shock ◽  
Strong Magnetic Fields ◽  
Random Forcing ◽  
Sturm Und Drang ◽  
Turbulent Dynamo ◽  
Starburst Regions

AbstractThe Galactic center central molecular zone (GCCMZ) bears similarities with extragalactic starburst regions, including a high supernova (SN) rate density. As in other starbursts like M82, the frequent SNe can heat the ISM until it is filled with a hot (∼ 4 × 107 K) superwind. Furthermore, the random forcing from SNe stirs up the wind, powering Mach 1 turbulence. I argue that a turbulent dynamo explains the strong magnetic fields in starbursts, and I predict an average B ∼70 μG in the GCCMZ. I demonstrate how the SN driving of the ISM leads to equipartition between various pressure components in the ISM. The SN-heated wind escapes the center, but I show that it may be stopped in the Galactic halo. I propose that the Fermi bubbles are the wind's termination shock.

scholarly journals The magnetic structure of our Galaxy: a review of observations

2008 ◽  
Vol 4 (S259) ◽  
pp. 455-466 ◽  
Author(s):  
JinLin Han
Keyword(s):  
Magnetic Fields ◽  
Magnetic Structure ◽  
Large Scale ◽  
Galactic Halo ◽  
Galactic Center ◽  
Galactic Plane ◽  
Galactic Disk ◽  
Dust Emission ◽  
Measure Data ◽  
Radio Sources

AbstractThe magnetic structure in the Galactic disk, the Galactic center and the Galactic halo can be delineated more clearly than ever before. In the Galactic disk, the magnetic structure has been revealed by starlight polarization within 2 or 3 kpc of the Solar vicinity, by the distribution of the Zeeman splitting of OH masers in two or three nearby spiral arms, and by pulsar dispersion measures and rotation measures in nearly half of the disk. The polarized thermal dust emission of clouds at infrared, mm and submm wavelengths and the diffuse synchrotron emission are also related to the large-scale magnetic field in the disk. The rotation measures of extragalactic radio sources at low Galactic latitudes can be modeled by electron distributions and large-scale magnetic fields. The statistical properties of the magnetized interstellar medium at various scales have been studied using rotation measure data and polarization data. In the Galactic center, the non-thermal filaments indicate poloidal fields. There is no consensus on the field strength, maybe mG, maybe tens of μG. The polarized dust emission and much enhanced rotation measures of background radio sources are probably related to toroidal fields. In the Galactic halo, the antisymmetric RM sky reveals large-scale toroidal fields with reversed directions above and below the Galactic plane. Magnetic fields from all parts of our Galaxy are connected to form a global field structure. More observations are needed to explore the untouched regions and delineate how fields in different parts are connected.

scholarly journals Large scale magnetic fields of our Galaxy

2009 ◽  
Vol 5 (H15) ◽  
pp. 450-451
Author(s):  
JinLin Han
Keyword(s):  
Star Formation ◽  
Magnetic Fields ◽  
Large Scale ◽  
Galactic Halo ◽  
Galactic Center ◽  
Galactic Plane ◽  
Galactic Disk ◽  
Zeeman Splitting ◽  
Radio Sources ◽  
Star Formation Regions

AbstractLarge-scale magnetic fields in the Galactic disk have been revealed by distributions of pulsar rotation measures (RMs) and Zeeman splitting data of masers in star formation regions, which have several reversals in arm and interarm regions. Magnetic fields in the Galactic halo are reflected by the antisymmetric sky distribution of RMs of extragalactic radio sources, which have azimuthal structure with reversed directions below and above the Galactic plane. Large-scale magnetic fields in the Galactic center probably have a poloidal and toroidal structure.

Interaction Between Magnetic Fields and Molecular Clouds on the Radio Arc

1990 ◽  
Vol 140 ◽  
pp. 381-381
Author(s):  
M. Tsuboi ◽  
T. Handa+ ◽  
M. Inoue ◽  
J. Inatani ◽  
N. Ukita
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Molecular Clouds ◽  
Galactic Center ◽  
Molecular Structures ◽  
Strong Magnetic Fields ◽  
Radio Observatory ◽  
Center Region ◽  
Supernova Explosions ◽  
The Magnetic Field

We have made observations of the Galactic center region in the CS J=1–0 and J=2–1 lines with the 45-m telescope at Nobeyama Radio Observatory in order to depict the fine structure and the activity of this region. We propose that several expanding molecular structures in this region are originated by successive supernova explosions at least of 102–3 times within 106 years. These may be responsible for strong magnetic fields in the Galactic center region. The interaction between one of the expanding molecular structures and the “vertical” filaments is found. From the appearance of the interaction, the magnetic field in the “vertical” filaments is estimated to be about 3–5 mGauss.

Strong magnetic fields

1960 ◽  
Vol 70 (4) ◽  
pp. 693-714 ◽  
Author(s):  
G.M. Strakhovskii ◽  
N.V. Kravtsov
Keyword(s):  
Magnetic Fields ◽  
Strong Magnetic Fields

Magnetic molecular nanoclusters in strong magnetic fields

2002 ◽  
Vol 172 (11) ◽  
pp. 1303 ◽  
Author(s):  
Anatolii K. Zvezdin ◽  
Viktor V. Kostyuchenko ◽  
V.V. Platonov ◽  
V.I. Plis ◽  
A.I. Popov ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Strong Magnetic Fields

scholarly journals The measurement of the energy of cosmic rays - II—The curvature measurements and the energy spectrum

1936 ◽  
Vol 154 (883) ◽  
pp. 573-587 ◽  
Keyword(s):  
Magnetic Field ◽  
Energy Spectrum ◽  
Cosmic Rays ◽  
Magnetic Fields ◽  
Strong Magnetic Fields ◽  
The Earth ◽  
Primary Particles ◽  
Curvature Measurements

Both the penetrating power of the cosmic rays through material ab­sorbers and their ability to reach the earth in spite of its magnetic field, make it certain that the energy of many of the primary particles must reach at least 10 11 e-volts. However, the energy measurements by Kunze, and by Anderson, using cloud chambers in strong magnetic fields, have extended only to about 5 x 10 9 e-volts. Particles of greater energy were reported, but the curvature of their tracks was too small to be measured with certainty. We have extended these energy measurements to somewhat higher energies, using a large electro-magnet specially built for the purpose and described in Part I. As used in these experiments, the magnet allowed the photography of tracks 17 cm long in a field of about 14,000 gauss. The magnet weighed about 11,000 kilos and used a power of 25 kilowatts.

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