Fast magnetic reconnection events can play an important role in accretion disk systems .
A potential model to explain the non-thermal very-high-energy ( VHE ) emission ( from GeV to TeV ) observed in black-hole binaries ( BHBs ) and Active Galatic Nuclei ( AGNs ) can be attributed to fast magnetic reconnection induced in the turbulent corona of accretion disks and/or jets .
In this work , we will discuss the results of global general relativistic MHD ( GRMHD ) simulations of accretion disks around black holes , whose turbulence is naturally driven by MHD instabilities , such as the magnetorotational instability ( MRI ) .
We will also present studies of magnetic reconnection driven by kink instabilities inside jets employing special relativistic MHD ( SRMHD ) simulations .
As we expect , our simulations reveal the development of a nearly steady-state turbulence driven by these instabilities .
We have performed a detailed statistical analysis to identify the presence of current sheets in the turbulent regions of both the accretion flow and jet .
We then determined the magnetic reconnection rates in these locations obtaining average reconnection velocities in Alfvén speed units of the order of 0.01 - 0.7 , which are consistent with the predictions of the theory of turbulence-induced fast reconnection .