We present images of the HH 211 molecular jet in the SiO v =0 , J =1–0 line at 43 GHz made with the Very Large Array at approximately 0.5 arcsec resolution .
The SiO emission appears to trace primarily internal bowshocks in the outflow , suggesting that the dust and molecular gas are accelerated via prompt entrainment at internal working surfaces in the jet .
There is also some evidence for limb-brightening of the SiO emission , indicating that SiO emission may also arise from entrainment in the jet ’ s boundary layer .
Excitation temperatures of \gtrsim 150 –200 K are inferred from the SiO emission .
Enhancements in the SiO abundance of \sim 10 ^ { 6 } over interstellar values are observed , and the possible origin of the SiO is discussed .