  We use N-body simulations of star clusters to investigate the possible
dynamical origins of the observed spread in core radius among intermediate-age
and old star clusters in the Large Magellanic Cloud (LMC). Two effects are
considered, a time-varying external tidal field and variations in primordial
hard binary fraction. Simulations of clusters orbiting a point-mass galaxy show
similar core radius evolution for clusters on both circular and elliptical
orbits and we therefore conclude that the tidal field of the LMC has not yet
significantly influenced the evolution of the intermediate-age clusters. The
presence of large numbers of hard primordial binaries in a cluster leads to
core radius expansion; however, the magnitude of the effect is insufficient to
explain the observations. Further, the range of binary fractions required to
produce significant core radius growth is inconsistent with the observational
evidence that all the LMC clusters have similar stellar luminosity functions.
