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Origin of Blazar Activity

Published online by Cambridge University Press:  25 May 2016

M. M. Romanova
M. M. Romanova*
Affiliation:
Space Research Institute of the Russian Academy of Sciences, Moscow, Russia; and Department of Astronomy, Cornell University, Ithaca, NY 14853-6801; [email protected]

Abstract

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Models of Blazars based on the propagation of finite discontinuities or fronts in the Poynting flux jet from the innermost regions of an accretion disk around a black hole are discussed. Such fronts may be responsible for short time–scale (from less than hours to days) flares in different wavebands from high frequency radioband to TeV, with delay in low radio frequencies as a result of synchrotron self-absorption. The cases of magnetic fields of one and opposite polarities across the front are investigated. We find that annihilation of magnetic field in the front leads to higher energy spectrum of leptons and possibility of strong TeV flares. Electron–positron pairs form in most cases as a result of interaction between numerous synchrotron photons and SSC photons, and constitute the majority species, compared with the ions at subparsec scales. Frequent weak outbursts may be responsible for flickering core radiation in all wavebands, while the stronger outbursts may be observed as short time–scale flares.

Type
III. AGN Theory and Models
Information
Symposium - International Astronomical Union , Volume 194: Activity in Galaxies and Related Phenomena , 1999 , pp. 256 - 268
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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