Non-thermal radiation associated with astrophysical shock waves

TL;DR

This thesis investigates the physical processes behind high-energy non-thermal emissions in various astrophysical objects, modeling gamma-ray production across different scales and source types to predict observable signals for current and future instruments.

Contribution

It introduces specific radiation models for gamma-ray emission in microquasars and active galactic nuclei, considering medium inhomogeneities and jet interactions, advancing predictive capabilities for high-energy astrophysics.

Findings

Models successfully predict gamma-ray emissions for different astrophysical sources.

Predictions are testable with current high-energy observatories like Fermi, AGILE, HESS, MAGIC, and CTA.

Enhanced understanding of particle acceleration and emission mechanisms in astrophysical shocks.

Abstract

The main goal of this thesis is to study the physical processes that can produce non-thermal emission at high energies in astrophysical objects capable to accelerate particles up to relativistic velocities. In particular, we have studied the gamma-ray emission produced in cosmic sources with different spatial scales, from young stellar objects to clusters of galaxies, going through microquasars and active galactic nuclei. In the former cases, we have modeled the gamma-ray emission using the radio data from the sources IRAS 16547-4247 and Abell 3376. In the latter, we have developed a specific radiation model based on the interaction of the inhomogeneities of the external medium with the jets generated by the compact object. Specifically, we have considered clumps of the massive stellar wind in microquasars, and clouds of the broad line region in active galactic nuclei, interacting with the jets of the sources. In all cases, the developed models allow us to make predictions testables with the new generation of instruments operating at high energies, such as the satellites Fermi and AGILE, and the Cherenkov telescopes HESS, MAGIC, and the forthcoming CTA.