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HH 212 is a nearby (400 pc) highly collimated protostellar jet powered by aClass 0 source in Orion. We have mapped the inner 80" (~ 0.16 pc) of the jet inSiO (J=8-7) and CO (J=3-2) simultaneously at ~ 0.5 resolution with the AtacamaMillimeter/Submillimeter Array at unprecedented sensitivity. The jet consistsof a chain of knots, bow shocks, and sinuous structures in between. As comparedto that seen in our previous observations with the Submillimeter Array, itappears to be more continuous, especially in the northern part. Some of theknots are now seen associated with small bow shocks, with their bow wingscurving back to the jet axis, as seen in pulsed jet simulations. Two of themare reasonably resolved, showing kinematics consistent with sideways ejection,possibly tracing the internal working surfaces formed by a temporal variationin the jet velocity. In addition, nested shells are seen in CO around the jetaxis connecting to the knots and bow shocks, driven by them. The proper motionof the jet is estimated to be ~ 115+-50 km/s, comparing to our previousobservations. The jet has a small semi-periodical wiggle, with a period of ~ 93yrs. The amplitude of the wiggle first increases with the distance from thecentral source and then stays roughly constant. One possible origin of thewiggle could be the kink instability in a magnetized jet.

Jet Motion, Internal Working Surfaces, and Nested Shells in the Protostellar System HH 212