Numerical simulations of dynamics and emission from relativistic astrophysical jets

TL;DR

This paper uses relativistic hydrodynamics and magnetohydrodynamics simulations to study the dynamics and emission of astrophysical jets from AGN and GRBs, providing insights into their physical properties and observational signatures.

Contribution

It introduces a comprehensive simulation framework combining relativistic fluid dynamics with radiative transfer to analyze jet behavior and emission across different astrophysical contexts.

Findings

Simulated jet dynamics match observed behaviors in AGN and GRBs.

The radiative transfer code accurately predicts multi-wavelength emission signatures.

Long-term simulations reveal evolution patterns of jet interaction with surrounding media.

Abstract

Broadband emission from relativistic outflows (jets) of active galactic nuclei (AGN) and gamma-ray bursts (GRBs) contains valuable information about the nature of the jet itself, and about the central engine which launches it. Using special relativistic hydrodynamics and magnetohydronamics simulations we study the dynamics of the jet and its interaction with the surrounding medium. The observational signature of the simulated jets is computed using a radiative transfer code developed specifically for the purpose of computing multi-wavelength, time-dependent, non-thermal emission from astrophysical plasmas. We present results of a series of long-term projects devoted to understanding the dynamics and emission of jets in parsec-scale AGN jets, blazars and the afterglow phase of the GRBs.