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 \pm 3 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 .