  A deep, continuum-subtracted, image of NGC 7293 has been obtained in the
light of the Halpha+[N II] emission lines. New images of two filamentary halo
stuctures have been obtained and the possible detection of a collimated outflow
made. Spatially resolved, longslit profiles of the Halpha+[N II] lines have
been observed across several of these features with the MES combined with the
SPM 2.1m telescope; these are compared with the [N II]6584, [O III]5007, HeII
6560 and Halpha profiles obtained over the nebular core. The central HeII
emission is originating in a ~0.34pc diameter spherical volume expanding at
<=12km/s which is surrounded, and partially coincident with an [O III] emitting
inner shell expanding at 12km/s. The bright helical structure surrounding this
inner region is modelled as a bi-polar nebula with lobe expansions of 25km/s
whose axis is tilted at 37deg to the sight line but with a toroidal waist
itself expanding at 14 km/s. These observations are compared with the
expectations of the interacting two winds model for the formation of PNe. Only
after the fast wind has switched off could this global velocity structure be
generated. Ablated flows must complicate any interpretation. It is suggested
that the clumpy nature of much of the material could play a part in creating
the radial `spokes' shown here to be apparently present close to the central
star. These `spokes' could in fact be the persistant tails of cometary globules
whose heads have now photo-evaporated completely. A halo arc projecting from
the north-east of the bright core has a conterpart to the south-east. Anomolies
in the position-velocity arrays of line profiles could suggest that these are
part of an expanding disc not aligned with the central helical structure though
expanding bi-polar lobes along a tilted axis are not ruled out.
