Study of relativistic particles and high energy emissions around black hole and jet sources through MHD, particle-in-cell (PIC) and radiative transfer

Abstract

In this research plan, we describe the general aspects of the theoretical and numerical techniques that we will employ to model the very high energy (VHE) emission from black hole (BH) environments and their associated jets, from microquasars to active galactic nuclei (AGN) scales. We will follow the fast magnetic reconnection scenario, developed by the supervisor ofthis project and her collaborators, who found that the magnetic power released from this model matches the observed emission of more than 230 sources (with BH masses spanning 10 order of magnitude) and also reproduces the spectral energy distribution (SED) of the sources, specially in the TeV range of gamma-ray emission. We aim to study magnetic reconnection in the coronal region of BH systems with 2-D and 3-D magnetohydrodynamic (MHD) simulations, and from these calculations try to reproduce the SED specially at VHE emission with test particle methods and radiative transfer codes. We will also explore magnetic reconnection acceleration along relativistic jets, combining particle-in-cell (PIC) and MHD approaches, in order to give a microscopic and macroscopicdescription of the plasma. With these results we aim to determine the conditions under which magnetic reconnection is more efficient than shocks to accelerate particles, and vice-versa.The outcomes of this study will provide predictions for the target sources to be detected with the Cherenkov Telescope Array (CTA) and ASTRI Mini- Array, the precursor of the CTA.With the theoretical and numerical tools employed for this project, we finally also aim to investigate potential magnetic reconnection events in magnetised massive stellar binaries, which could be applied to interpret gamma-ray emission from star forming regions. (AU)