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We present new adaptive optics echelle spectra of the near-infrared [Fe II]lines in the redshifted and blueshifted jets from the T Tauri star RW Aur. Thespectra have an unprecedented combination of high spatial and spectralresolution that makes it possible to trace the dynamics of the flow to aprojected distance of only 10 AU from the source. As noted by previous studies,the redshifted flow is much slower than its fainter blueshifted counterpart.Our observations clearly show that both the radial velocities and the emissionline widths are larger closer to the source on both sides of the jet. The linewidths are 20% - 30% of the jet velocity on both sides of the flow,significantly larger than would be produced by a divergent constant velocityflow. The observed line widths could arise from a layered velocity structure inthe jet or from magnetic waves. A bright knot in the redshifted jet has noconcomitant increase in line width, implying that it is not heated by a bowshock. Alternate heating mechanisms include planar shocks, ambipolar diffusionand magnetic reconnection.

Adaptive Optics Echelle Spectroscopy of [Fe II] 1.644 um in the RW Aur Jet: A Narrow Slice Down the Axis of the Flow