12-20 July 2017
BEXCO
Asia/Seoul timezone
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Contribution

BEXCO - Room F(201/202/203/204)

[GA298] Magnetic reconnection at the core region of non-blazar AGNs and their multi-wavelength emission

Speakers

  • Pankaj KUSHWAHA

Primary authors

  • Pankaj KUSHWAHA (IAG, University of Sao Paulo, Sao Paulo 05508-900, Brazil)

Co-authors

Description

The origin of the very high energy (VHE) emission from non-blazar sources, like radio galaxies, is still debated. The compactness of the emission regions - as inferred from high-variability flux observations - suggests that the emission may come from the non-screened core region at the jet launching. Recently, it has been shown that the power released by fast magnetic reconnection driven by turbulence can explain the emission from such sources and also accelerate particles to relativistic energies via first-order Fermi process. Using the power released in this model and a non-thermal particle spectrum, we show that the multi-wavelength emission from radio-galaxies can be successfully explained within a leptonic-hadronic scenario from radio to TeV gamma-rays. We confirm that most of the VHE emission escapes from the coronal region around the black hole/ accretion disk without producing electron-positron pairs and the size of the region required is also consistent with the observed fast temporal variability. Thus, the reproduction of multi-wavelength emission naturally identifies turbulent induced magnetic reconnection at the core (or jet launching basis) of these low luminous galaxies as one of the possible processes. This scenario is also consistent, at least qualitatively, with recent numerical GRMHD simulations of accretion disks around black holes.