http://arxiv.org/abs/2102.04193
Radio galaxies play an important role in the seeding of cosmic rays and magnetic fields in galaxy clusters. Here, we simulate the evolution of relativistic electrons injected into the intracluster medium by radio galaxies. Using passive tracer particles added to magnetohydrodynamical adaptive-mesh simulations, we calculate the evolution of the spectrum of relativistic electrons taking into account energy losses and re-acceleration mechanisms associated with the dymamics of the intracluster medium. Re-acceleration can occur at shocks via diffusive shock acceleration, and in turbulent flows via second-order Fermi re-acceleration. Relativistic electrons from radio galaxies are found to fill the intracluster medium over scales of several $100 \rm ~Myr$, and they create a stable reservoir of fossil electrons which remains available for further re-acceleration by shock waves and turbulent gas motions. In the near future, deep radio observations (especially at low frequencies) are likely to probe such mechanisms in galaxy clusters.
F. Vazza, D. Wittor, G. Brunetti, et. al.
Tue, 9 Feb 21
57/87
Comments: 20 pages, 18 figures, submitted to A & A
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