  We present 3D hydrodynamical simulations of an isotropic fast wind
interacting with a previously ejected toroidally-shaped slow wind in order to
model both the observed morphology and the kinematics of the planetary nebula
(PN) NGC 6302. This source, also known as the Butterfly nebula, presents one of
the most complex morphologies ever observed in PNe. From our numerical
simulations, we have obtained an intensity map for the H$\alpha$ emission to
make a comparison with the Hubble Space Telescope (HST) observations of this
object. We have also carried out a proper motion (PM) study from our numerical
results, in order to compare with previous observational studies. We have found
that the two interacting stellar wind model reproduces well the morphology of
NGC 6302, and while the PM in the models are similar to the observations, our
results suggest that an acceleration mechanism is needed to explain the
Hubble-type expansion found in HST observations.
