A comparison between observed and theoretical H-R diagrams for the young LMC star cluster NGC 1866
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Abstract
A scheme for constructing synthetic H-R diagrams as a function of cluster age, metallicity, and He abundance from a three-dimensional grid of theoretical evolutionary tracks in Y, Z, and mass is outlined. This scheme is then applied to fit observed color-magnitude data for the LMC star cluster NGC 1866. This comparison between theory and observation provides both a sensitive test of the stellar evolution models and a means to determine the age and composition of the cluster. The best fit to the cluster data is for a composition of (Y, Z) = (0.273 + or - 0.010, 0.0160 + or - 0.0008) and an age of 86 + or - 5 x 10 to the 6th yr, with an intrinsic dispersion in age of less than 5 x 10 to the 6th yr. The population of Cepheids is also computed. Sources of uncertainty in the data and theory are discussed, and the possible importance of nonlocal convection processes is highlighted.
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