The simulations demonstrate that the properties and patterns of the relativistic particle populations and emissions are fundamentally influenced by the inherently unsteady behavior of jet flows. In particular, since the terminal jet shock is neither steady nor plane, relativistic electrons accelerated there exhibit a range of properties, both spatially and temporally within the jet terminal hot spot and the back-flow cocoon. Simple, fluid-based models of synchrotron emission in radio galaxies can provide a useful first impression of expected radio properties. However, it is also clear that careful inclusion of physical information about the distinct spatial and momentum distributions of the radiating electrons can add considerable valuable information about dynamics within the flows and local conditions. An electron population is fed in with the jet.
Diffusive acceleration takes place at strong shocks.
High tones are large. Click here for an animation. For electron density, high tones are large. For electron spectrum, high tones are flat Flat spectra are a consequence of acceleration at shocks. The complex electron spectral distribution results from the complex behavior of the terminal shock.