The Role of Fast Magnetic Reconnection on the Radio and Gamma-Ray Emission from the Nuclear Regions of Microquasars and Low Luminosity AGNs and Black Hole Binaries and the Origin of their Gamma-Ray Emission

Abstract

Fast magnetic reconnection can be a very powerful mechanism operating in the core region of black hole binaries (BHBs) and active galactic nuclei (AGNs). In earlier work, we have been suggested that the power released by fast reconnection events between the magnetic field lines lifting from the inner accretion disk region and the lines anchored into the central black hole (BH) could accelerate relativistic particles in a first-order Fermi process and produce the observed radio emission from BHBs and low luminosity AGNs (LLAGNs). Moreover, we have been proposed that the observed correlation between the radio emission and the mass of these sources, spanning 10 10 orders of magnitude in mass, might be related to this process. Here we present our late results of the comparison of the magnetic power released by fast reconnection with the observed very high energy emission (from MeV/GeV to Tev bands) of BHBs, LLAGNs, blazars, and gammaray bursts (GRBs). In the case of LLAGNs and BHBs, not only the radio but also the gamma-ray emission can be due to magnetic power released by fast reconnection and follows the same trend in the luminosity-mass diagram as that of the core radio emission of these sources (tested for over 200 sources). This indicates that the very high energy emission of these sources can be produced in the core. On the other hand, the emission from blazars and GRBs does not follow the same trend, suggesting that their emission is produced outside the core, as expected. PoS(ICRC2015)919Fast Magnetic Reconnection in the Core Region of LLAGNs and BHBs Luís H. S. Kadowaki Figure 1: Schematic drawing of the magnetic field geometry in the region surrounding the BH. R X characterizes the inner accretion disk radius. ∆R X and L X correspond to the width and the extension of the magnetic reconnection region, respectively. L is the height of the corona. Obtained from [11].