A study of the wiggle morphology of HH 211 through numerical simulations

TL;DR

This study uses 3D hydrodynamic simulations to replicate the wiggle morphology of the HH 211 protostellar jet, supporting the binary motion hypothesis and providing insights into jet dynamics and observational signatures.

Contribution

It demonstrates that binary-induced jet source motion can produce the observed wiggle, and offers detailed simulation results matching SMA observations of HH 211.

Findings

Wiggle morphology can be reproduced by binary motion at the jet source.

A sinusoidal velocity variation approximates observed knot patterns.

Complex velocity structures suggest caution in interpreting radial velocity data.

Abstract

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.