Using numerical simulations in the context of a simple dissipative model (Abadi et al. 1990) we study the final morphologies and dynamical properties of galaxies under different initial conditions. The protogalaxies are embedded in dynamically relaxed potential wells of dark matter with different initial spin parameters λ and velocity dispersions σ in the dissipative component. We find that both λ and σ control the final morphology of the galaxies. The angular momentum might be acquired by tidal torques, and several sources may account for the velocity dispersion. For instance, under the assumption that supernovae explosions provide kinetic energy to the medium giving σ ∼ 8-10 km/s (Mc Kee & Ostriker 1977) our models suggest that the border line spin parameter between early type and late type morphologies would be approximately λ ∼ 0.04.