  The rate of galaxy cluster eccentricity evolution is useful in understanding
large scale structure. Rapid evolution for $z < $ 0.13 has been found in two
different observed cluster samples. We present an analysis of projections of 41
clusters produced in hydrodynamic simulations augmented with radiative cooling
and 43 clusters from adiabatic simulations. This new, larger set of simulated
clusters strengthens the claims of previous eccentricity studies. We find very
slow evolution in simulated clusters, significantly different from the reported
rates of observational eccentricity evolution. We estimate the rate of change
of eccentricity with redshift and compare the rates between simulated and
observed clusters. We also use a variable aperture radius to compute the
eccentricity, r$_{200}$. This method is much more robust than the fixed
aperture radius used in previous studies. Apparently radiative cooling does not
change cluster morphology on scales large enough to alter eccentricity. The
discrepancy between simulated and observed cluster eccentricity remains.
Observational bias or incomplete physics in simulations must be present to
produce halos that evolve so differently.
