Synchrotron brightness distribution of turbulent radio jets

Details Synchrotron brightness distribution of turbulent radio jets Synchrotron brightness distribution of turbulent radio jets

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...257...63h&link_type=abstract

Astrophysical Journal, Part 1, vol. 257, June 1, 1982, p. 63-74. Research supported by the Natural Sciences and Engineering Res

Astronomy and Astrophysics

Astronomy

33

Brightness Distribution, Galactic Radiation, Radio Jets (Astronomy), Relativistic Particles, Synchrotron Radiation, Turbulent Jets, Galactic Structure, Magnetohydrodynamic Waves, Mathematical Models, Particle Acceleration, Radio Astronomy, Turbulent Mixing

Scientific paper

Radio jets are considered as turbulent mixing regions and it is proposed that the essential small scale viscous dissipation in these jets is by emission of MHD waves and by their subsequent strong damping due, at least partly, to gyro-resonant acceleration of supra-thermal particles. A formula relating the synchrotron surface brightness of a radio jet to the turbulent power input is deduced from physical postulates, and is tested against the data for NGC315 and 3C31 (NGC383). The predicted brightness depends essentially on the collimation behavior of the jet, and, to a lesser extent, on the CH picture of a 'high' nozzle with accelerating flow. The conditions for forming a large scale jet at a high nozzle from a much smaller scale jet are discussed. The effect of entrainment on the prediction is discussed with the use of similarity solutions. Although entrainment is inevitably associated with the turbulent jet, it may or may not be a dominant factor depending on the ambient density profile.

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