Modelling blazar flaring using a time-dependent fluid jet emission model
  - an explanation for orphan flares and radio lags
  Blazar jets are renowned for their rapid violent variability and
multiwavelength flares, however, the physical processes responsible for these
flares are not well understood. In this paper we develop a time-dependent
inhomogeneous fluid jet emission model for blazars. We model optically thick
radio flares for the first time and show that they are delayed with respect to
the prompt optically thin emission by ~ months to decades, with a lag that
increases with the jet power and observed wavelength. This lag is caused by a
combination of the travel time of the flaring plasma to the optically thin
radio emitting sections of the jet and the slow rise time of the radio flare.
We predict two types of flares: symmetric flares - with the same rise and decay
time, which occur for flares whose duration is shorter than both the radiative
lifetime and the geometric path-length delay timescale; extended flares - whose
luminosity tracks the power of particle acceleration in the flare, which occur
for flares with a duration longer than both the radiative lifetime and
geometric delay. Our model naturally produces orphan X-ray and $\gamma$-ray
flares. These are caused by flares which are only observable above the
quiescent jet emission in a narrow band of frequencies. Our model is able to
successfully fit to the observed multiwavelength flaring spectra and
lightcurves of PKS1502+106 across all wavelengths, using a transient flaring
front located within the broad-line region.
