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Characterization of the binary fractions in star clusters is of fundamentalimportance for many fields in astrophysics. Observations indicate that themajority of stars are found in binary systems, while most stars with massesgreater than $0.5 M_\odot$ are formed in star clusters. In addition, sincebinaries are on average more massive than single stars, in resolved starclusters these systems are thought to be good tracers of (dynamical) masssegregation. Over time, dynamical evolution through two-body relaxation willcause the most massive objects to migrate to the cluster center, while therelatively lower-mass objects remain in or migrate to orbits at greater radii.This process will globally dominate a cluster's stellar distribution. However,close encounters involving binary systems may disrupt `soft' binaries. Thisprocess will occur more frequently in a cluster's central, dense region than inits periphery, which may mask the effects of mass segregation. Using highresolution Hubble Space Telescope observations, combined with sophisticated$N$-body simulations, we investigate the radial distributions of themain-sequence binary fractions in massive young Large Magellanic Cloud starclusters. We show that binary disruption may play an important role on veryshort timescales, depending on the environmental conditions in the clustercores. This may lead to radial binary fractions that initially decline in thecluster centers, which is contrary to the effects expected from dynamical masssegregation.

The dynamical importance of binary systems in young massive star clusters