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The two Large Magellanic Cloud star clusters NGC 1805 and NGC 1818 areapproximately the same chronological age (~30 Myr), but show different radialtrends in binary frequency. The F-type stars (1.3 - 2.2 MSun) in NGC 1818 havea binary frequency that decreases towards the core, while the binary frequencyfor stars of similar mass in NGC 1805 is flat with radius, or perhaps bimodal(with a peak in the core). We show here, through detailed N-body modeling, thatboth clusters could have formed with the same primordial binary frequency andwith binary orbital elements and masses drawn from the same distributions(defined from observations of open clusters and the field of our Galaxy). Theobserved radial trends in binary frequency for both clusters are best matchedwith models that have initial substructure. Furthermore, both clusters may beevolving along a very similar dynamical sequence, with the key difference thatNGC 1805 is dynamically older than NGC 1818. The F-type binaries in NGC 1818still show evidence of an initial period of rapid dynamical disruptions (whichoccur preferentially in the core), while NGC 1805 has already begun to recovera higher core binary frequency, owing to mass segregation (which willeventually produce a distribution in binary frequency that rises only towardsthe core, as is observed in old Milky Way star clusters). This recovery rateincreases for higher-mass binaries, and therefore even at one age in onecluster, we predict a similar dynamical sequence in the radial distribution ofthe binary frequency as a function of binary primary mass.

Different Dynamical Ages for the Two Young and Coeval LMC Star Clusters NGC 1805 and NGC 1818 Imprinted on Their Binary Populations