Abstract:
The origin of γ-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 γ-ray bright blazars, 3C 279 (z = 0.54) and 3C 454.3 (z = 0.86),
using near-simultaneous radio-to-γ-ray observations. For both sources, the γ-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 γ-ray flares.
