Ponente
Descripción
Radio-loud Active Galactic Nuclei (AGN) produce relativistic jets that are among the most energetic structures in the universe. These jets emit radiation across most of the electromagnetic spectrum, with their Spectral Energy Distribution (SED) typically exhibiting a double hump structure. The lower energy part of the SED is dominated by synchrotron emission from non-thermal electrons in the jet. Observations of AGN jets have also revealed complex, time-dependent morphologies that span vast length scales. To understand the morphology, dynamics, and evolution of these jets, it is essential to model their physical properties, such as density, energy and magnetic field. This study uses the PLUTO code to perform 3D relativistic magnetohydrodynamic (RMHD) simulations of kiloparsec-scale jet morphologies. The resulting morphology is investigated for three different jet velocities: a relativistic, mildly relativistic, and non-relativistic case. The synchrotron emission is modelled for each simulation using Lagrangian particles that represent the non-thermal electron population. The electron spectrum is evolved over time, accounting for effects such as diffusive shock acceleration and radiative cooling. A post-processing ray-tracing code is used to generate intensity maps and polarisation vectors by integrating the emission coefficients of each simulation cell along arbitrary lines of sight. The code accounts for both relativistic effects as well as light travel time. The results reveal emission features corresponding to recollimation shocks within the jet beam, which in some cases produce multiple bright components along the jet axis. Additionally, it is shown that magnetic filaments in the jet cocoon can reproduce filamentary emission similar to that observed in the lobes of FR II-type radio galaxies.
