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Fast TeV variability in blazars: jets in a jet

Dimitrios Giannios2Max Planck Institute for Astrophysics, Box 1317, D-85741 Garching, GermanyDmitri A. Uzdensky1Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544, USAMitchell C. Begelman4Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309, USA

2009en

Ochiq kirishYashil

ABI

Annotatsiya

Abstract The fast TeV variability of the blazars Mrk 501 and PKS 2155−304 implies a compact emitting region that moves with a bulk Lorentz factor of Γem∼ 100 towards the observer. The Lorentz factor is clearly in excess of the jet Lorentz factors Γj≲ 10 measured on sub-pc scales in these sources. We propose that the TeV emission originates from compact emitting regions that move relativistically within a jet of bulk Γj∼ 10. This can be physically realized in a Poynting flux-dominated jet. We show that if a large fraction of the luminosity of the jet is prone to magnetic dissipation through reconnection, then material outflowing from the reconnection regions can efficiently power the observed TeV flares through synchrotron-self-Compton emission. The model predicts simultaneous far-ultraviolet/soft X-ray flares.

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Identifikatorlar

DOI: 10.1111/j.1745-3933.2009.00635.x

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