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Although the giant radiogalaxy M 87 harbors many distinct regions ofbroad-band nonthermal emission, the recently reported fast variability of TeVgamma rays from M 87 on a timescale of days strongly constrains the range ofspeculations concerning the possible sites and scenarios of particleacceleration responsible for the observed TeV emission. A natural productionsite of this radiation is the immediate vicinity of the central supermassivemass black hole (BH). Because of the low bolometric luminosity, the nucleus ofM 87 is effectively transparent for gamma rays up to energy of 10 TeV, whichmakes this source an ideal laboratory for study of particle accelerationprocesses close to the BH event horizon. We critically analyse differentpossible radiation mechanisms in this region, and argue that the observed veryhigh-energy gamma ray emission can be explained by the inverse Compton emissionof ultrarelativistic electron-positron pairs produced through the developmentof an electromagnetic cascade in the BH magnetosphere. We demonstrate, throughdetailed numerical calculations of acceleration and radiation of electrons inthe magnetospheric vacuum gap, that this ``pulsar magnetosphere like'' scenariocan satisfactorily explain the main properties of TeV gamma-ray emission of M87.

Production of TeV gamma-radiation in the vicinity of the supermassive black hole in the giant radiogalaxy M87