Jets and hotspots in extragalactic radio sources

Abstract

Radio gaps, i.e. regions of strongly reduced radio (and also optical) intensity between the galactic nucleus (AGN) and the radio jets in active radio galaxies are a rather prominent feature of many of these sources (Bridle, 1986). With the aim to explain this phenomenon we consider the evolution of the relativistic electron spectrum in such a source with the relevant plasma kinetic equations. We consider a possible acceleration process for relativistic electrons and positrons near the accreting central object which is based on the continuous interplay of stochastic Fermi acceleration processes and radiation losses of energetic particles (Schlickeiser, 1984). The resulting distribution function heats the background medium effectively through the oblique Langmuir synchrotron instability (Lesch et al., 1989a) once the threshold plasma energy density for the modulation instability is exceeded resulting in the outflow of material. By the concerted action of synchrotron losses and adiabatic focussing in the ordered, spatially decaying magnetic field B0 the isotropic relativistic electron distribution function rapidly develops into to oppositely directed beam distributions, explaining the formation of compact, superluminal radio jets near the AGN and the radio gap phenomenon. The stability of the electron/positron beam in the magnetized background plasma is studied by treating it as a cold beam. The linear growth rates for parrallel propagating longitudinal and transversal waves are calculated. Whereas the former give rise to heating of the background plasma, the low-frequency transversal (Alfven-) waves scatter the beam to an isotropic distribution function which then reveals itself again by synchrotron radiation. A lower limit for the mean free path for this isotropization process is calculated and compared with the length of the radio gaps. A discussion of the results is given.