  Recent high-resolution high-sensitivity observations of protostellar jets
have shown many to possess deviations to their trajectories. HH 211 is one such
example where sub-mm observations with the SMA have revealed a clear
reflection-symmetric wiggle. The most likely explanation is that the HH 211 jet
source could be moving as part of a protobinary system. Here we test this
assumption by simulating HH 211 through 3D hydrodynamic jet propagation
simulations using the PLUTO code with a molecular chemistry and cooling module,
and initial conditions based on an analytical model derived from SMA
observations. Our results show the reflection-symmetric wiggle can be recreated
through the assumption of a jet source perturbed by binary motion at its base,
and that a regular sinusoidal velocity variation in the jet beam can be close
to matching the observed knot pattern. However, a more complex model with
either additional heating from the protostar, or a shorter period velocity
pulsation may be required to account for enhanced emission near the source, and
weaker knot emission downstream. Position velocity diagrams along the pulsed
jet beam show a complex structure with detectable signatures of knots and show
caution must be exercised when interpreting radial velocity profiles through
observations. Finally, we make predictions for future HH 211 observations with
ALMA.
