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The current detectors of gamma-ray emission specially at TeV energies havetoo poor resolution to determine whether this emission is produced in the jetor in the core, particularly of low luminous, non-blazar AGNs (like radiogalaxies). In recent works it has been found that the power released by eventsof turbulent fast magnetic reconnection in the core region of these sources ismore than sufficient to reproduce the observed gamma-ray luminosities. Besides,3D MHD simulations with test particles have demonstrated that a first-orderFermi process within reconnection sites with embedded turbulence results veryefficient particle acceleration rates. We computed here the spectral energydistribution (SED) from radio to gamma-rays of the radio galaxies for whichenergy emission up to TeVs has been detected (namely, M87, Cen A, Per A, and IC310). For this aim, we employed the acceleration model above and considered allthe relevant leptonic and hadronic loss processes around the core region of thesources. We found that the calculated SEDs match very well specially with theVHE observations, therefore strengthening the conclusions above in favour of acore emission origin for the VHE emission of these sources. The model alsonaturally explains the observed very fast variability of the VHE emission.

Particle Acceleration and gamma-ray emission due to magnetic reconnection around the core region of radio galaxies