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Ultrafast VHE Gamma-Ray Flares of IC 310

Published online by Cambridge University Press:  23 June 2017

Maxim V. Barkov ,
Felix Aharonian  and
Dmitriy V. Khangulyan
Maxim V. Barkov
Affiliation:
DESY, Platanenallee 6, 15738 Zeuthen, Germany email: maxim.barkov@desy.de Astrophysical Big Bang Laboratory, RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan email: maxim.barkov@riken.jp
Felix Aharonian
Affiliation:
Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-69117 Heidelberg, Germany
Dmitriy V. Khangulyan
Affiliation:
Department of Physics, Rikkyo University, Nishi-Ikebukuro 3-34-1, Toshima-ku, Tokyo 171-8501, Japan
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Abstract

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In 2012 November MAGIC detected a bright flare from IC 310. The flare consisted of two sharp peaks with a typical duration of ~ 5 min. The energy released during that event has been estimated to be at the level of 2 × 1044 erg s−1.

In this work we derive an upper limit on the possible luminosity of flares generated in black hole (BH) magnetosphere, which depends very weakly on the mass of BH and is determined by disk magnetisation, viewing angle, and pair multiplicity. Since all these parameters are smaller than a unit, the luminosity 2 × 1043 erg s−1 can be taken as a strict upper limit for flare luminosity for several minutes variability time. This upper limit appears to be approximately an order of magnitude below the value measured with MAGIC. Thus, we conclude that it seems very unfeasible that the magnetospheric processes can be indeed behind the bright flaring activity recorded from IC 310.

Keywords

gamma rays: theorygalaxies: activegalaxies: active
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S324: New Frontiers in Black Hole Astrophysics , September 2016 , pp. 157 - 163
Copyright
Copyright © International Astronomical Union 2017 

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