Dynamical Evolution of Open Star Clusters of Varying Initial Mass Functions in STARLAB

N-body simulations are widely used to model the dynamical evolution of a variety of systems, among them star clusters. Much of our understanding of star cluster evolution rests on the results of N-body simulations, providing insight in the structural evolution of these systems, as well as a detailed study of mass segregation. Observations show that the more massive members of a star cluster aggregate toward the center, while less massive members tend to move farther away from the center. Using the N-body code STARLAB/KIRA we construct a large number of open star cluster models with various initial mass functions: a Saltpeter mass function (power law with exponent $\alpha= -2.35$), a series of additional power law functions with each exponent increasing by 0.2 from the last ($\alpha = -2.15,-1.95,-1.75$) and a Miller-Scalo mass function. For each mass function, we simulate an ``ensemble'' of 160 individual clusters each containing 2600 stars. We compare the time evolution within these simulations to models that begin with mass segregation by combining two different simulated clusters. With a ``hybrid'' of the two dynamical models we perform a comparison to determine what effect joining together simulations has on cluster evolution and our ability to replicate observational data.