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Star clusters are the building blocks of galaxies. They are composed of starsof nearly equal age and chemical composition, allowing us to use them aschronometers and as testbeds for gauging stellar evolution. It has become clearrecently that massive stars are formed preferentially in close binaries, inwhich mass transfer will drastically change the evolution of the stars. This isexpected to leave a significant imprint in the distribution of cluster stars inthe Hertzsprung-Russell diagram. Our results, based on a dense model grid ofmore than 50,000 detailed binary-evolution calculations, indeed show severaldistinct, coeval main-sequence (MS) components, most notably an extended MSturnoff region, and a group of near-critical rotating stars that is spread overa large luminosity range on the red side of the classical MS. Wecomprehensively demonstrate the time evolution of the features in an animation,and we derive analytic expressions to describe these features. We findquantitative agreement with results based on recent photometric andspectroscopic observations. We conclude that while other factors may also be atplay, binary evolution has a major impact on the MS morphology of young starclusters.

Effects of close binary evolution on the main-sequence morphology of young star clusters