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Nonthermal radio emission from the Galaxy

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Abstract

Synchrotron radio emission from interstellar space has long been recognized as a useful tool to probe into the galactic distribution of high energy electrons and magnetic fields. We first review the results obtained from the local (<2kpc distant) region of the Galaxy and conclude that the observed local synchrotron emissivity is consistently explained by the measured cosmic ray electron spectrum and the interstellar magnetic field if some reasonable assumptions are allowed. The large scale distribution of radio emissivity shows evidence for spiral structure and is likely to originate in two distinct disk systems: a thin disk (thickness 250 pc in the inner Galaxy) formed by population I objects which emits about 10% of the galactic radio luminosity and a thick disk (2.5 kpc thick in the inner Galaxy) which constitutes the truly diffuse emission and produces 90% of the total luminosity.

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Authors and Affiliations

  1. Max-Planck-Institut für Physik und Astrophysik, Institut für extraterrestrische Physik, 8046, Garching, Germany

    G. Kanbach

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  1. G. Kanbach
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Proceedings of the XVIII General Assembly of the IAU: Galactic Astrophysics and Gamma-Ray Astronomy, held at Patras, Greece, 19 August 1982.

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Kanbach, G. Nonthermal radio emission from the Galaxy. Space Sci Rev 36, 273–283 (1983). https://doi.org/10.1007/BF00247092

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  • DOI: https://doi.org/10.1007/BF00247092

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