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We attempt to explain the observed radio and gamma-ray emission produced inthe surrounds of black holes by employing a magnetically-dominated accretionflow (MDAF) model and fast magnetic reconnection triggered by turbulence. Inearlier work, standard disk model was used and we refine the model by focussingon the sub-Eddington regime to address the fundamental plane of black holeactivity. The results do not change substantially with regard to previous workensuring that the details of the accretion physics are not relevant in themagnetic reconnection process occurring in the corona. Rather our work putsfast magnetic reconnection events as a powerful mechanism operating in the coreregion, near the jet base of black hole sources on more solid ground. Formicroquasars and low-luminosity active galactic nuclei (LLAGNs) the observedcorrelation between radio emission and mass of the sources can be explained bythis process. The corresponding gamma-ray emission also seems to be produced inthe same core region. On the other hand, the emission from blazars andgamma-ray bursts (GRBs) cannot be correlated to core emission based on fastreconnection.

On the role of fast magnetic reconnection in accreting black hole sources