The Accretion Disc-Jet Connection in Blazars
  The power spectral density (PSD) of the X-ray emission variability from the
accretion disc-corona region of black hole X-ray binaries and active galactic
nuclei has a broken power law shape with a characteristic break time-scale. If
the disc and the jet are connected, the jet variability may also contain a
characteristic time-scale related to that of the disc-corona. Recent
observations of the blazar Mrk 421 have confirmed the broken power law shape of
the PSD of its jet X-ray variability. We model the time variability of a
blazar, in which emitting particles are assumed to be accelerated by successive
shock waves flowing down the jet with a varying inter-shock time-scale. We
investigate the possible relation between the characteristic time-scales in the
disc and jet variability based on the above model, along with mathematically
and physically simulated disc variability. We find that both the PSD of the jet
and disc variability may have a broken power law shape but the break
time-scales are not related in general except only in systems with a small
range of BH mass. The break in the jet and the disc PSD are connected to the
interval between large amplitude outbursts in the jet (inter-shock time-scale)
and to the viscous time-scale in the disc, respectively. In frequency bands
where multiple emission processes are involved or emission is from lower energy
particles, the break in the PSD may not be prominent enough for detection.
