Abstract
With the adoption of the synchrotron self-Compton (SSC) + external Compton (EC) model, investigation has been conducted on the radiation mechanisms of the GeV-bright active galaxy GB 1310+487 through modeling its quasi-simultaneous spectral energy distributions in active and quiescent states. We find that from the flare states to the post-flare state, the magnetic field (B) has experienced a gradual increase, whereas the electron spectrum’s prefactor (N0) and break energy () decrease accordingly. The model indicates that the energy of the Poynting flux may be used to accelerate electrons. As for the GeV emission in the source, it is dominated by the EC process while the SSC contribution is negligible. Varying energy distribution of the emitting electrons, rather than location of the radiation blob, appears to be the driving factor for the observed changes in EC emission. Despite the similar total jet power and the same likely energy carrier (cold protons), the radiation efficiency of GB 1310+487 is lower than what is found in bright Fermi blazars.
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