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On the Origin of Gamma-ray Flares from Bright Fermi Blazars
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The origin of gamma-ray flares observed from blazars is one of the major mysteries in jet physics. We have attempted to address this problem following a novel spectral energy distribution (SED) fitting technique that explored the flaring patterns identified in the broadband SEDs of two gamma-ray bright blazars 3C 279 (z=0.54) and 3C 454.3 (z=0.86), using near-simultaneous radio-to-gamma-ray observations. For both sources, the gamma-ray flux strongly correlates with the separation of the SED peaks and the Compton dominance. We propose that spectral hardening of the radiating electron population and/or enhancement of the Doppler factor can naturally explain these observations. In both cases, magnetic reconnection may play a pivotal role in powering the luminous gamma-ray flares.
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Deciphering the Multi-Wavelength Flares of the Most Distant Very High-Energy (>100 GeV) Gamma-ray Emitting Blazar
A one-zone leptonic model with torus-dominated external Compton radiation reproduces the multi-wavelength spectra of OP 313 in five states, placing the gamma-ray emission between the BLR and the dusty torus.
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