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Numerical study of magnetic reconnection around black hole

Grant number: 16/12320-8
Support type:Scholarships in Brazil - Post-Doctorate
Effective date (Start): March 01, 2017
Effective date (End): February 28, 2019
Field of knowledge:Physical Sciences and Mathematics - Astronomy
Principal Investigator:Elisabete Maria de Gouveia Dal Pino
Home Institution: Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG). Universidade de São Paulo (USP). São Paulo, SP, Brazil
Associated research grant:13/10559-5 - Investigation of high energy and plasma astrophysics phenomena: theory, numerical simulations, observations, and instrument development for the Cherenkov Telescope Array (CTA), AP.TEM


Fast magnetic reconnection events can be a very powerful mechanism operating in the core region of active galactic nuclei (AGN) and microquasars. In earlier work, we have suggested that the power released by reconnection events between the magnetic field lines lifting from the accretion disk and those anchored into the horizon of black holes (BH) could produces jets and accelerate relativistic particles in a first-order Fermi process and produce the observed radio and gamma-ray emission from microquasars and low luminosity AGNs (LLAGNs). Moreover, we have shown that the observed correlation between the radio and gamma-ray emission and the mass of the central BH of these sources, spanning 10^10 orders of magnitude in mass, might be related to this mechanism. These studies highlight the importance of the magnetic reconnection in the nuclear region of compact sources whose origin at high energies, in the TeV band, is still a subject of intense discussion in the literature. Since a numerical study is required to prove the viability of fast magnetic reconnection events in these systems, this project aims to carry out radiative transfer calculations and magnetohydrodynamic simulations (involving a general relativistic approximation) of accretion disks systems with corona and a central BH. A study of the interaction between the magnetosphere of the BH and the magnetic field of the coronal region will allow us to verify the occurrence of magnetic reconnection events and the connection of these with particle acceleration and jet formation. We will also combine these numerical studies with the high energy radiative processes that are produced in the vicinity of these compact sources, which will allow us to make realistic predictions for the observations of the light curves and spectral energy distributions (SEDs), up to 100 TeVs, which will be obtained for the first time with the new generation of gamma-ray telescopes, namely the ASTRI Mini-Array and the Cherenkov Telescope Array (CTA). (AU)