We calculated a model to investigate the shaping of a PN morphological group, i.e. elliptical PNe, in terms of the so-called Interacting Winds Model. The angle-dependent mass loss generated by a dust driven wind due to a slow rotation of the AGB star is an effective way for the shaping of PNe. The matter which is more concentrated in the equatorial region of the star influences the flow of the fast hot wind originating from the central star, resulting in elliptical or weakly bipolar shapes for the corresponding PNe. A wide range of elliptical shapes can be explained by this model. In contrast to previous studies the angle-dependent mass loss on the AGB is not parameterized by an arbitrary formula but is taken from self-consistent dust-driven wind models. Furthermore we discuss the influence of the different inclination of the PNe in the sky, the interaction with an inhomogenous interstellar medium and the possible effect of a magnetic field in or around the old AGB star. Using detailed morphology studies with the Hubble Space Telescope (HST) we discuss possible scenarios to explain the sometimes very complex structures.
A&A 354, 573