Angular Momentum of Protogalaxies in a Hierarchical Scenario

We use numerical simulations of collisionless particles in expanding universe models with different density parameters {OMEGA} in order to simulate local mass density enhancements in a {OMEGA}_b_ = 1 background. We find an anticorrelation of the intrinsic spin of bound objects with the local density. The average dimensionless spin parameter of virialized objects in present high-density regions ρ\ρ_b_ ~10^3^ is a factor of 2 lower than that corresponding to objects in the field. The implications for galaxy formation and the segregation of morphological types are briefly discussed.