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Upon their formation, dynamically cool (collapsing) star clusters will,within only a few million years, achieve stellar mass segregation for starsdown to a few solar masses, simply because of gravitational two-bodyencounters. Since binary systems are, on average, more massive than singlestars, one would expect them to also rapidly mass segregate dynamically.Contrary to these expectations and based on high-resolution Hubble SpaceTelescope observations, we show that the compact, 15-30 Myr-old LargeMagellanic Cloud cluster NGC 1818 exhibits tantalizing hints at the >= 2 sigmalevel of significance (> 3 sigma if we assume a power-law secondary-to-primarymass-ratio distribution) of an increasing fraction of F-star binary systems(with combined masses of 1.3-1.6 Msun) with increasing distance from thecluster center, specifically between the inner 10 to 20" (approximatelyequivalent to the cluster's core and half-mass radii) and the outer 60 to 80".If confirmed, this will offer support of the theoretically predicted but thusfar unobserved dynamical disruption processes of the significant population of'soft' binary systems---with relatively low binding energies compared to thekinetic energy of their stellar members---in star clusters, which we haveaccess to here by virtue of the cluster's unique combination of youth and highstellar density.

Gravitational conundrum? Dynamical mass segregation versus disruption of binary stars in dense stellar systems