Broadband modelling of Orphan gamma ray flares

Blazars, a class of highly variable active galactic nuclei, sometimes exhibit Orphan γ-ray flares. These flares having high flux only in energies do not show significant variations at lower energies. We study the temporal and spectral profile these detail from three γ−ray bright blazars, 3C 273, PKS 1510-089 279 also their simultaneous broadband emissions. find that variability timescales were (0.96±0.28) days, (3.12±2.40) hr (2.16±0.72) hr, for 279, respectively. The energy distributions (SEDs) during have been modelled with leptonic model two emission regions. This suggests might originated inverse Compton scattering relativistic electrons by seed photons broad-line region or dusty torus, which is first region. While second broader region, lying further down jet, could be responsible X-ray radio possible locations regions jets sources estimated SED modelling.