  We have used the technique of spectro-astrometry to study the milli-arcsecond
scale structure of the emission lines in the T Tauri star RU Lupi. The wings of
the H-alpha emission are found to be displaced from the star towards the
south-west (blue wing) and north-east (red wing) with angular scales of 20-30
milli-arcsecs. This structure is consistent with a bipolar outflow from the
star. From a study of the variability of the intensity and position spectra we
argue that a combination of magnetically-driven bipolar outflow and accreting
gas contribute to the H-alpha emission. On the other hand, the [OI] and [SII]
emission are displaced from the star to the south-west but at much larger
distances than the H-alpha, hundreds of milli-arcsecs for the high-velocity
component (HVC) and down to 30 milli-arcsecs for the low-velocity components
(LVC). The presence of both red-shifted and blue-shifted outflows in H-alpha
but only a blue-shifted outflow in the forbidden lines can be explained if the
disc obscures the red-shifted forbidden line outflow, but a disc gap with outer
radius 3-4 au allows the red-shifted H-alpha to be seen. This gap could be
induced by an unseen companion.
