Synchrotron radiation spectrum for galactic-sized plasma filaments

Details Synchrotron radiation spectrum for galactic-sized plasma filaments Synchrotron radiation spectrum for galactic-sized plasma filaments

Feb 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990itps...18...49p&link_type=abstract

IEEE Transactions on Plasma Science (ISSN 0093-3813), vol. 18, Feb. 1990, p. 49-55.

Astronomy and Astrophysics

Astrophysics

4

Background Radiation, Birkeland Currents, Cosmic Plasma, Cosmic Rays, Emission Spectra, Synchrotron Radiation, Biot Method, Filaments, Maxwell-Boltzmann Density Function, Thermal Plasmas

Scientific paper

The radiation spectrum for synchrotron-emitting electrons in galactic-sized Birkeland current filaments is analyzed. It is shown that the number of filaments required to thermalize the emission spectrum to blackbody is not reduced when a non-Maxwellian electron distribution is assumed. If the cosmic background radiation (CBR) spectrum (T = 2.76 K) is due to absorption and re-emission of radiation from galactic-sized current filaments, higher-order synchrotron modes are not as highly self-absorbed as lower-order modes, resulting in a distortion of the blackbody curve at higher frequencies. This is especially true for a non-Maxwellian distribution of electrons for which the emission coefficient at high frequencies is shown to be significantly less than that for a Maxwellian distribution. The deviation of the CBR spectrum in the high-frequency regime may thus be derivable from actual astrophysical parameters, such as filamentary magnetic fields and electron energies in the model.

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