Numerical simulations of the internal shock model in magnetized relativistic jets of blazars

TL;DR

This paper uses numerical simulations to study how magnetization affects the internal shock model in relativistic jets of blazars, aiming to better understand their emission variability.

Contribution

It introduces a high-performance parallel code to simulate magnetized shell collisions and systematically analyzes the impact of magnetization on observed radiation in blazar jets.

Findings

Magnetization significantly influences spectral energy distributions.

Shell collision dynamics are altered by magnetic fields.

The model reproduces diverse light-curve patterns.

Abstract

The internal shocks scenario in relativistic jets is used to explain the variability of the blazar emission. Recent studies have shown that the magnetic field significantly alters the shell collision dynamics, producing a variety of spectral energy distributions and light-curves patterns. However, the role played by magnetization in such emission processes is still not entirely understood. In this work we numerically solve the magnetohydodynamic evolution of the magnetized shells collision, and determine the influence of the magnetization on the observed radiation. Our procedure consists in systematically varying the shell Lorentz factor, relative velocity, and viewing angle. The calculations needed to produce the whole broadband spectral energy distributions and light-curves are computationally expensive, and are achieved using a high-performance parallel code.