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We report the results of a study of cluster density profiles using n-body simulations. The results for cosmologies with $\Omega_o = 1.0; \Omega_o = 0.2$; and $\Omega_o = 0.2, \lambda_o = 0.8$ are compared for initial power spectra $P(k) = Ak^n$, where $n = -2, -1, 0$. We note distinct differences between these cosmologies and show that the $\Omega$-dependence of the profile slope is not masked by the $n$-dependence. We also demonstrate the inadequacy of certain simple models, notably flat core models, in fitting the profiles.
