Nonthermal Radio Emission of the Galaxy and the Origin of Cosmic Radiations.

1956 ◽  
Vol 123 ◽  
pp. 491 ◽  
Author(s):  
C. Y. Fan
Keyword(s):  
Radio Emission ◽  
Nonthermal Radio ◽  
The Galaxy ◽  
Nonthermal Radio Emission

scholarly journals Radial distributions of constituents in M33, the Galaxy, and M51

1985 ◽  
Vol 106 ◽  
pp. 431-434
Author(s):  
Elly M. Berkhuijsen ◽  
Ulrich Klein
Keyword(s):  
Radio Emission ◽  
Blue Light ◽  
Column Density ◽  
Surface Brightness ◽  
Far Infrared ◽  
Abundance Ratio ◽  
Nonthermal Radio ◽  
The Galaxy ◽  
Nonthermal Radio Emission

The radial distributions of the surface brightness or column density of thermal and nonthermal radio emission, far-infrared (FIR) emission, blue light, HI and CO in the Sc galaxies M33 and M51 are compared with the corresponding distributions in the Galaxy. Information on the variation of the absorption at Hα and on the variation of the abundance ratio O/H is also shown.

Spectrum of nonthermal radio emission from the galaxy. Observations at frequencies of 200 and 375 MHz

1983 ◽  
Vol 26 (9) ◽  
pp. 769-777
Author(s):  
P. P. Belyaev ◽  
A. F. Tarasov ◽  
Yu. V. Tokarev ◽  
M. A. Yurishchev
Keyword(s):  
Radio Emission ◽  
Nonthermal Radio ◽  
The Galaxy ◽  
Nonthermal Radio Emission

scholarly journals On the Relationship Between Recent Measurements of Cosmic Ray Electrons, Nonthermal Radio Emission from the Galaxy, and the Solar Modulation of Cosmic Rays

1968 ◽  
Vol 21 (6) ◽  
pp. 845 ◽  
Author(s):  
WR Webber
Keyword(s):  
Cosmic Rays ◽  
Radio Emission ◽  
Electron Spectrum ◽  
Cosmic Ray ◽  
Solar Modulation ◽  
Nonthermal Radio ◽  
The Galaxy ◽  
Nonthermal Radio Emission ◽  
Modulation Parameter ◽  
The Relationship

Utilizing recent measurements of the cosmic ray electron spectrum at the Earth and the effects of solar modulation on this spectrum, possible limits on the local interstellar electron spectrum have been determined. Synchrotron emission from these interstellar electrons is then compared with the local (disk) volume emissivity of nonthermal radio emission as deduced from a study of radio intensity profiles along the galactic equator. The detailed spectrum and magnitude of radio emissivity can be reproduced from the electron spectrum only for very stringent, conditions on the magnitude of the local interstellar magnetic field, and the amount of solar modulation of cosmic rays. Specifically it is found that B -L "'" 7 !-,G, and the residual modulation parameter KR "'" 0�75 GV. If solar modulation effects on the cosmic ray electron component are negligible then an implausibly high local field of "'" 20 !-,G is required.

scholarly journals On the Nature of the Galactic Halo

1958 ◽  
Vol 8 ◽  
pp. 935-939
Author(s):  
S. B. Pickelner ◽  
I. S. Shklovsky
Keyword(s):  
Radio Emission ◽  
Velocity Dispersion ◽  
Galactic Halo ◽  
Rarefied Gas ◽  
Magnetic Energy ◽  
Density Fluctuations ◽  
Spherical System ◽  
Nonthermal Radio ◽  
The Galaxy ◽  
Nonthermal Radio Emission

In 1952 it was shown by one of us that the sources of galactic nonthermal radio emission form a nearly spherical system concentrating toward the plane and the center of the galaxy. It was pointed out independently by the other author that the field between the clouds must be sufficiently strong to retain the cosmic rays in the galaxy. The density of the kinetic energy of the gas between the clouds could be taken as equal to that of the magnetic energy. Thus the velocity dispersion of the rarefied gas in the space between the clouds should be large and form a spherical, not a flat, subsystem. The spherical distribution of the radio emission supports this suggestion. The wide H and K absorption lines appearing in the spectra of early supergiants are also an argument in favor of the reality of fast movements of the rarefied gas. However, L. Spitzer points out that at least a part of these lines belong to the stars. Spectrograms taken by G. Münch show that some of the wide lines consist of a few faint narrow lines. These phenomena may be explained by the density fluctuations of rarefied gas (kv ∝ n2), but some other interpretations are also possible. This phenomenon supports the hypothesis that the more rarefied gas possesses a higher velocity dispersion. The existence of wide H and K lines is not the principal argument of this theory. It will be shown below that the gas of the halo is too rarefied to give observable lines.

Detection of Nonthermal Radio Emission from Coronal X-Ray Jets

1995 ◽  
Vol 447 (2) ◽  
Author(s):  
M. R. Kundu, ◽  
J. P. Raulin, ◽  
N. Nitta, ◽  
H. S. Hudson, ◽  
M. Shimojo, ◽  
...  
Keyword(s):  
Radio Emission ◽  
X Ray ◽  
Nonthermal Radio ◽  
Nonthermal Radio Emission

scholarly journals Magnetic annihilation in colliding-wind binary systems

1995 ◽  
Vol 163 ◽  
pp. 523-524
Author(s):  
M. Jardine ◽  
H.R. Allen ◽  
A.M.T. Pollock
Keyword(s):  
Particle Acceleration ◽  
Radio Emission ◽  
Magnetic Reconnection ◽  
Stagnation Point ◽  
Binary Systems ◽  
Nonthermal Radio ◽  
Nonthermal Radio Emission ◽  
Reconnection Model

We investigate the possibility that a stagnation-point magnetic reconnection model may account for the particle acceleration necessary for the generation of nonthermal radio emission in the Wolf-Rayet binary systems exemplified by WR140.

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