Multiple shell planetary nebulae (MSPNe) are those which, in addition to the main bright inner shell, show one or two additional external shells. These faint external shells often have aspherical geometries, indicating an interaction with the surrounding interstellar medium (ISM). Our aim is to investigate, first of all, if the current theoretical stellar evolutionary models are able to reproduce the different observed shells and secondly, which ISM conditions are necessary in order to see the effect of a moving central star in the PN halo. We have performed hydrodynamical simulations following the evolution of the stellar winds predicted by the theoretical stellar evolutionary models. The study has been done in two parts: first, we approach the problem of the formation of multiple shells in the case of a star at rest, then we investigate the interaction of the different shells with the ISM due to a moving central star.