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Fast magnetic reconnection events can be a very powerful mechanism operatingat the jet launching region of microquasars and AGNs. We have recently foundthat the power released by reconnection between the magnetic field lines of thecoronal inner disk region and the lines anchored into the black hole is able toaccelerate relativistic particles through a first-order Fermi process andproduce the observed radio luminosity from both microquasars and low luminousAGNs (LLAGNs). We also found that the observed correlation between the radioluminosity and the mass of these sources, spanning 10^9 orders of magnitude inmass, is naturally explained by this process. In this work, assuming that thegamma-ray emission is probably originated in the same acceleration zones thatproduce the radio emission, we have applied the scenario above to investigatethe origin of the high energy outcomes from an extensive number of sourcesincluding high (HLAGNs) and LLAGNs, microquasars and GRBs. We find correlationof our model with the gamma emission only for microquasars and a few LLAGNs,while none of the HLAGNs or GRBs are fitted, neither in radio nor in gamma. Weattribute the lack of correlation of the gamma emission for most of the LLAGNsto the fact that this processed emission doesn't depend only on the localmagnetic field activity around the source/accretion disk, but also on otherenvironmental factors like the photon and density fields. We conclude that theemission from the LLAGNs and microquasars comes from the nuclear region oftheir sources and therefore, can be driven by nuclear magnetic activity.However, in the case of the HLAGNs and GRBs, the nuclear emission is blocked bythe surrounding density and photon fields and therefore, we can only see thejet emission further out.

The role of fast magnetic reconnection in acceleration zones of microquasars and AGNs