Turbulent generation of magnetic fields in extended extragalactic radio sources

1980 ◽  
Vol 241 ◽  
pp. 81 ◽  
Author(s):  
D. S. de Young
Keyword(s):  
Magnetic Fields ◽  
Radio Sources ◽  
Extragalactic Radio Sources

scholarly journals 9.10. The cause of the spectral turnover in the GPS source 0108+388: free-free absorption or SSA?

1998 ◽  
Vol 184 ◽  
pp. 401-402
Author(s):  
J. M. Marr ◽  
F. Crawford ◽  
G. B. Taylor
Keyword(s):  
Magnetic Fields ◽  
Radio Source ◽  
High Frequency ◽  
Radio Sources ◽  
Host Galaxies ◽  
Ionized Gas ◽  
High Frequencies ◽  
Extragalactic Radio Sources ◽  
Competing Models ◽  
Frequency Radiation

The radio source 0108 + 388 is a canonical example of a class of extragalactic radio sources, referred to as Gigahertz-Peaked Spectrum (GPS) sources, whose spectra peak at high frequencies. There are two competing models for the cause of the high frequency turnover: free-free absorption (f-f) of the lower frequency radiation by ionized gas in the host galaxies (e.g. van Breugel 1984), or synchrotron self-absorption (SSA) due to exceptionally large magnetic fields, (e.g. Hodges, Mutel, & Phillips 1984).

scholarly journals On the Magnetic Fields of Galaxies

2021 ◽  
pp. 470-477
Author(s):  
R. R. Andreasyan
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Faraday Rotation ◽  
Radio Galaxies ◽  
Morphological Properties ◽  
Radio Sources ◽  
Extragalactic Radio Sources

We bring results of some our investigations of magnetic field of our Galaxy and extragalactic radio sources. For the study were used data of Faraday rotation of pulsars and extragalactic radio sources as well as data of physical and morphological properties of more than 500 radio galaxies of different morphological classes.

scholarly journals Radio polarization effects in the Galaxy

1964 ◽  
Vol 20 ◽  
pp. 143-147
Author(s):  
F. F. Gardner
Keyword(s):  
Magnetic Fields ◽  
Background Radiation ◽  
Radio Sources ◽  
Polarization Effects ◽  
Galactic Magnetic Fields ◽  
Extragalactic Radio Sources ◽  
The Galaxy ◽  
Galactic Radiation

Polarization effects involving our Galaxy have been studied in two ways: firstly, by observations of the polarization of the galactic radiation itself, and secondly, by the effects of galactic magnetic fields and ionization on the polarization of extragalactic radio sources. For an aerial of fixed dimensions, the intensity of the background varies at about λ2·5 (λ is wavelength) and that of the sources at about λ0·7. Thus background measurements are restricted to the longer wavelengths where the radiation is sufficiently intense, while sources are most easily studied at the shorter wavelengths where background confusion is small. The background radiation includes a component from small unresolved extragalactic radio sources in addition to the galactic radiation which is of interest in the first type of measurement. Both types of observation have been made with the 210-foot aerial at Parkes; the observations of sources were done in collaboration with J. B. Whiteoak and that of the galactic radiation with J. A. Roberts, assisted by J. B. Whiteoak and A. G. Little for part of the time.

scholarly journals Proton-Proton Collisions in Extragalactic Radio Sources

1982 ◽  
Vol 97 ◽  
pp. 75-76 ◽  
Author(s):  
S. E. Okoye ◽  
P. N. Okeke
Keyword(s):  
Magnetic Fields ◽  
Point Of View ◽  
Low Energy ◽  
Radio Sources ◽  
Relativistic Electrons ◽  
Proton Proton ◽  
Proton Collisions ◽  
Extragalactic Radio Sources ◽  
Inverse Compton ◽  
Proton Proton Collisions

The majority of extragalactic radio sources are known to consist of two extended components straddling an optical galaxy or quasar with each component being maintained from the nucleus of the associated optical object through a beam or jet of relativistic plasma and magnetic fields. Hitherto, the energetics of radio source components have been considered essentially from the point of view of the cooling of the relativistic electrons through their interaction with ambient magnetic fields (synchrotron radiation) and with low energy photons (inverse Compton emission). Here we consider a hitherto neglected problem involving the mutual interactions between the fast particles themselves. (The results of a detailed investigation into these interactions will be reported elsewhere — see Okoye and Okeke, 1982.)

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