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Blazars, a class of highly variable active galactic nuclei, sometimes exhibitOrphan $\gamma$-ray flares. These flares having high flux only in $\gamma$-rayenergies do not show significant variations in flux at lower energies. We studythe temporal and spectral profile of these Orphan $\gamma$-ray flares in detailfrom three $\gamma-ray$ bright blazars, 3C 273, PKS 1510-089 and 3C 279 andalso their simultaneous broadband emissions. We find that the variabilitytimescales of the Orphan $\gamma$-ray flares were $(0.96\pm0.28)$ days,$(3.12\pm2.40)$ hr and $(2.16\pm0.72)$ hr, for 3C 273, PKS 1510-089 and 3C 279,respectively. The broadband spectral energy distributions (SEDs) during theseflares have been modelled with a leptonic model from two emission regions. Thismodel suggests that Orphan $\gamma$-ray flares might have originated frominverse Compton scattering of relativistic electrons by the seed photons fromthe broad-line region or dusty torus, which is the first region. While thesecond broader region, lying further down the jet, could be responsible forX-ray and radio emissions. The possible locations of these emission regions inthe jets of the three sources have been estimated from SED modelling.

Broadband Modelling of Orphan Gamma Ray Flares