A New Potential-Density Pair for Spherical Star Systems

I present a new potential-density pair for use in computational simulations of spherically symmetric star systems. My model contains a finite-density core and results in an r^-4 density falloff at large radii. I produce velocity dispersion profiles for five different Milky Way globular clusters, and compare them to dispersion profiles constructed from observational data. These results are also checked against the Plummer model to examine their relative accuracies. I find that both models are in great agreement with observation, producing dispersion profiles that match collected data to a high degree.