Modeling the Emission from Turbulent Relativistic Jets in Active
  Galactic Nuclei
  We present a numerical model developed to calculate observed fluxes of
relativistic jets in active galactic nuclei. The observed flux of each
turbulent eddy is dependent upon its variable Doppler boosting factor, computed
as a function of the relativistic sum of the individual eddy and bulk jet
velocities and our viewing angle to the jet. The total observed flux is found
by integrating the radiation from the eddies over the turbulent spectrum. We
consider jets that contain turbulent eddies that have either standard
Kolmogorov or recently derived relativistic turbulence spectra. We also account
for the time delays in receiving the emission of the eddies due to their
different simulated positions in the jet, as well as due to the varying beaming
directions as they turn over. We examine these theoretical light curves and
compute power spectral densities (PSDs) for a range of viewing angles, bulk
velocities of the jet, and turbulent velocities. These PSD slopes depend
significantly on the turbulent velocity and are essentially independent of
viewing angle and bulk velocity. The flux variations produced in the
simulations for realistic values of the parameters tested are consistent with
the types of variations observed in radio-loud AGN as, for example, recently
measured with the Kepler satellite, as long as the turbulent velocities are not
too high.
