Here we present a new approach for constraining luminous blazars , incorporating fully time-dependent and self-consistent modeling of bright \gamma -ray flares of PKS 1510-089 resolved with Fermi -LAT , in the framework of the internal shock scenario .
The results of our modeling imply the location of the \gamma -ray flaring zone outside of the broad-line region , namely around \simeq 0.3 pc from the core for a free-expanding jet with the opening angle \Gamma \theta _ { \mathrm { jet } } \simeq 1 ( where \Gamma is the jet bulk Lorentz factor ) , up to \simeq 3 pc for a collimated outflow with \Gamma \theta _ { \mathrm { jet } } \simeq 0.1 .
Moreover , under the \Gamma \theta _ { \mathrm { jet } } \simeq 1 condition , our modeling indicates the maximum efficiency of the jet production during the flares , with the total jet energy flux strongly dominated by protons and exceeding the available accretion power in the source .
This is in contrast to the quiescence states of the blazar , characterized by lower jet kinetic power and an approximate energy equipartition between different plasma constituents .
We demostrate how strictly simultaneous observations of flaring PKS 1510–089 at optical , X-ray , and GeV photon energies on hourly timescales , augmented by extensive simulations as presented in this paper , may help to impose further precise constraints on the magnetization and opening angle of the emitting region .
Our detailed modeling implies in addition that a non-uniformity of the Doppler factor across the jet , caused by the radial expansion of the outflow , may lead to a pronounced time distortion in the observed \gamma -ray light curves , resulting in particular in asymmetric flux profiles with substantially extended decay phases .