We present hydrodynamical simulations of multiple shell planetary nebulae (MSPN) formation using evolutionary models of 1, 1.5, 2, 2.5, 3.5 and 5 M_odot. Stellar evolution from the AGB (Vassiliadis & Wood 1993) to the post-AGB phase (Vassiliadis & Wood 1994) was followed. Included in our simulations are the effect of stellar evolution and fast wind. The hardening of the stellar spectra as the central star moves across the H-R diagram is also taken into account. The formation of detached haloes as consequence of thermal pulses during the AGB is investigated as well as the effects of the ionization front on the formation of attached shells. Comparison with observations is also shown. Hydrodynamical simulation were carried out with the MHD code ZEUS-3D.