We present a flexible interactive 3D morpho-kinematical modeling application for astrophysics. Compared to other systems, our application reduces the restrictions on the physical assumptions, data type, and amount that is required for a reconstruction of an object's morphology. It is one of the first publicly available tools to apply interactive graphics to astrophysical modeling. The tool allows astrophysicists to provide a priori knowledge about the object by interactively defining 3D structural elements. By direct comparison of model prediction with observational data, model parameters can then be automatically optimized to fit the observation. The tool has already been successfully used in a number of astrophysical research projects.
Based on axisymmetric hydrodynamical simulations and three-dimensional (3D) reconstructions with Shape, we investigate the kinematical signatures of deviations from homologous (Hubble-type) outflows in some typical shapes of planetary nebulae (PNs). We find that, in most situations considered in our simulations, the deviations from a Hubble-type flow are significant and observable. The deviations are systematic and a simple parameterization of them considerably improves morphokinematical models of the simulations. We describe such extensions to a homologous expansion law that capture the global velocity structure of hydrodynamical axisymmetric nebulae during their wind-blown phase. It is the size of the poloidal velocity component that strongly influences the shape of the position-velocity diagrams that are obtained, not so much the variation of the radial component. The deviations increase with the degree of collimation of the nebula and they are stronger at intermediate latitudes. We describe potential deformations which these deviations might produce in 3D reconstructions that assume Hubble-type outflows. The general conclusion is that detailed morphokinematical observations and modeling of PNs can reveal whether a nebula is still in a hydrodynamically active stage (windy phase) or whether it has reached ballistic expansion.  On a obtenu les champs des vitesses d'expansion [OIII] et Hα dans les nebuleuses planetaires NGC 6058 et 6804 et les champs des vitesses d'expansion [OIII], Hα et [NII] dans NGC 6309 6751 et 6818, a partir de spectres de haute dispersion. On a obtenu des modeles spatiocinematiques des nebuleuses en supposant une vitesse d'expansion du gaz proportionnelle a la distance a l'etoile centrale et en utilisant la correlation entre le rayon et la vitesse d'expansion donnee par Sabbadin et coll. (1984)