  We present a detailed analysis of time- and energy-dependent synchrotron
polarization signatures in a shock-in-jet model for gamma-ray blazars. Our
calculations employ a full 3D radiation transfer code, assuming a helical
magnetic field throughout the jet. The code considers synchrotron emission from
an ordered magnetic field, and takes into account all light-travel-time and
other relevant geometric effects, while the relevant synchrotron self-Compton
and external Compton effects are taken care of with the 2D MCFP code. We
consider several possible mechanisms through which a relativistic shock
propagating through the jet may affect the jet plasma to produce a synchrotron
and high-energy flare. Most plausibly, the shock is expected to lead to a
compression of the magnetic field, increasing the toroidal field component and
thereby changing the direction of the magnetic field in the region affected by
the shock. We find that such a scenario leads to correlated synchrotron + SSC
flaring, associated with substantial variability in the synchrotron
polarization percentage and position angle. Most importantly, this scenario
naturally explains large PA rotations by > 180 deg., as observed in connection
with gamma-ray flares in several blazars, without the need for bent or helical
jet trajectories or other non-axisymmetric jet features.
