Broadband modelling of Orphan gamma ray flares

Abstract

Blazars, a class of highly variable active galactic nuclei, sometimes exhibit Orphan γ-ray flares. These flares having high flux only in γ-ray energies do not show significant variations in flux at lower energies. We study the temporal and spectral profile of these Orphan γ-ray flares in detail from three γ−raybright blazars, 3C273, PKS1510-089 and 3C279 and also their simultaneous broadband emissions. We find that the variability timescales of the Orphan γ-ray flares were (0.96 ±0.28)days, (3.12 ±2.40)hr and (2.16 ±0.72)hr, for 3C273, PKS1510-089 and 3C279, respectively. The broadband spectral energy distributions (SEDs) during these flares have been modelled with a leptonic model from two emission regions. This model suggests that Orphan γ-ray flares might have originated from inverse Compton scattering of relativistic electrons by the seed photons from the broad-line region or dusty torus, which is the first region. While the second broader region, lying further down the jet, could be responsible for X-ray and radio emissions. The possible locations of these emission regions in the jets of the three sources have been estimated from SED modelling.