Ponente
Descripción
The internal structure and dynamics of relativistic jets in active galactic nuclei (AGN) are central to understanding where and how particles are accelerated to very high energies. In particular, recollimation shocks and the turbulent regions they generate downstream can serve as natural sites for localized energy dissipation and non-thermal particle energization. Using high-resolution 2D and 3D relativistic magnetohydrodynamic (RMHD) simulations with the PLUTO code, we explore how the jet’s macroscopic structure—shaped by external confinement, pressure gradients between the jet and its environment, and the structure of the magnetic field—governs the development of time-dependent features that can efficiently accelerate particles. Our results provide a physically grounded framework connecting the large-scale dynamics of AGN jets to their spectral, polarization, and variability signatures in the very-high-energy (VHE) regime. This work offers new insights into the emission of high-energy-peaked blazars, highlighting the importance of global jet modeling for interpreting VHE observations.
