Simulating the dynamics and synchrotron emission from relativistic jets – II. Evolution of non-thermal electrons

ABSTRACT We have simulated the evolution of non-thermal cosmic ray electrons (CREs) in 3D relativistic magneto hydrodynamic (MHD) jets evolved up to a height 9 kpc. The CREs been space and energy concurrently with jet fluid, duly accounting for radiative losses acceleration at shocks. show that stable MHD instabilities expected trends regular flow spine hotspot followed by settling backflow. However, unstable create complex shock structures head (kink instability), spine-cocoon interface, cocoon itself (Kelvin–Helmholtz modes). after exiting undergo further crossings such scenarios are re-accelerated cocoon. different trajectories turbulent cocoons evolutionary history spectral parameters. Thus, same spatial location, there is mixing CRE populations, resulting total spectrum when averaged over given area. Cocoons can an excess build energetic due re-acceleration turbulence driven shocks slowed expansion decelerated jet. This will add budget