2015/04/28 by Khiali, Behrouz, E. M. de Gouveia Dal Pino, Pino, Elisabete M. de Gouveia Dal +3
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Particle Detector Development and Performance #Neutrino Physics Research
paper · pdf · doi:10.48550/arxiv.1504.07592
The current detectors of gamma-ray emission specially at TeV energies have\ntoo poor resolution to determine whether this emission is produced in the jet\nor in the core, particularly of low luminous, non-blazar AGNs (like radio\ngalaxies). In recent works it has been found that the power released by events\nof turbulent fast magnetic reconnection in the core region of these sources is\nmore than sufficient to reproduce the observed gamma-ray luminosities. Besides,\n3D MHD simulations with test particles have demonstrated that a first-order\nFermi process within reconnection sites with embedded turbulence results very\nefficient particle acceleration rates. We computed here the spectral energy\ndistribution (SED) from radio to gamma-rays of the radio galaxies for which\nenergy emission up to TeVs has been detected (namely, M87, Cen A, Per A, and IC\n310). For this aim, we employed the acceleration model above and considered all\nthe relevant leptonic and hadronic loss processes around the core region of the\nsources. We found that the calculated SEDs match very well specially with the\nVHE observations, therefore strengthening the conclusions above in favour of a\ncore emission origin for the VHE emission of these sources. The model also\nnaturally explains the observed very fast variability of the VHE emission.\n