![]() ![]() Denoting the variability time-scale as \(\Delta t=60\Delta \)(1 + z) −1. ![]() Recent detections of minute-scale gamma-ray variability in blazar light curves imply limits on the sizes of the high-energy emission region that challenge the shock-in-jet scenario 9, 10, 11. The time-variability of the emission at the highest frequencies allows to witness the physical processes going on in the innermost parts of the jets 9. Shock acceleration, however, may not be efficient in the magnetically dominated relativistic plasma 7, 8. It is commonly believed that the emission is produced by ultra-relativistic particles accelerated at shock waves travelling down the jet 6. The relativistic motion of the plasma boosts the non-thermal jet emission into a forward cone. It is not known yet how and where the energy of the twisted magnetic fields near the black hole is converted into the kinetic energy of the particles in the jet 5.īlazars are commonly understood as jets emerging from AGN viewed under small angles with the line of sight. The recent Event Horizon Telescope (EHT) 3 observation of the active galactic nucleus (AGN) M 87 provides corroborating evidence for this scenario 4. Accreting black holes are suspected to convert rotational energy into Poynting flux escaping along their rotation axes and powering collimated jets 1, 2. ![]()
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