They are characterized by predominantly radial motions in theiroutermost parts, but also incorporate an extended flattened region which rotates coherently about a well-virializedcore of triaxial shape with an approximately isotropic velocity dispersion. We characterize the kinematical anddynamical properties of these complex velocity fields and we briefly discuss the possible relevance of thesesimple toy models to the observed structure of real galaxies, emphasizing the difference between dissipative anddissipationless disk formation.