NGC 2440 : A morpho-kinematical model
  This work describes the modelling of the 3D structure and position-velocity
(P-V) diagrams of NGC 2440, a well known planetary nebula, aiming to describe
the morphology of this object, specially its core. We have used high resolution
spectra and P-V diagrams to reproduce the 3D structure of the nebula using
SHAPE, a software that allows 3D modelling. HST high angular resolution images
were used as reference to the model.
  The observational data point to a segmented core, and the simulations confirm
this assumption; the best model for the nebula is a torus segmented in three
pieces. The simulated P-V diagrams agree with the observations. We suggest that
the torus was torn apart by interaction with the surrounding medium, either as
winds or the radiation field.
  For the two bipolar lobes, orientation angles to the plane of the sky of
$27\pm$5 and $-5\pm3$ degrees, respectively for the bipolar components with PA
of 85 and 35 degrees, were derived. No additional bipolar lobes were required
to model the observed features of NGC 2440. A distance of $1.8 \pm 0.5$ kpc was
derived for the nebula using our velocity field for the toroidal structure.
These results are the first derived for NGC 2440 from modelling in a 3D
environment.
