  In this study we use simulations of 128$^3$ particles to study the
ellipticity and orientation of clusters of galaxies in N-body simulations of
differing power-law initial spectra (P(k) \propto k^n ,n = +1, 0, -1, -2$), and
density parameters ($\Omega_0 = 0.2$ to 1.0). Furthermore, unlike most
theoretical studies we mimic most observers by removing all particles which lie
at distances greater than 2 1/h Mpc from the cluster center of mass.
  We computed the axial ratio and the principal axes using the inertia tensor
of each cluster. The mean ellipticity of clusters increases strongly with
increasing $n$. We also find that clusters tend to become more spherical at
smaller radii.
  We compared the orientation of a cluster to the orientation of neighboring
clusters as a function of distance (correlation). In addition, we considered
whether a cluster's major axis tends to lie along the line connecting it to a
neighboring cluster, as a function of distance (alignment). Both alignments and
correlations were computed in three dimensions and in projection to mimic
observational surveys. Our results show that significant alignments exist for
all spectra at small separations ($D < 15 h^{-1}$ Mpc) but drops off at larger
distance in a strongly $n-$dependent way.
