Binary interaction dominates the evolution of massive stars. Towards the field binary population: influence of orbital decay on close binaries. Evolution towards the critical limit and the origin of Be stars. Stellar spin rates of O-type spectroscopic binaries. Spin-down of protostars through gravitational torques. Stellar mergers as the origin of magnetic massive stars. Formation of close binaries by disc fragmentation and migration, and its statistical modelling. Effects of close binary evolution on the main-sequence morphology of young star clusters. Evolution of mass functions of coeval stars through wind mass loss and binary interactions. On the origin of the bimodal rotational velocity distribution in stellar clusters: rotation on the pre-main sequence. The effects of binary stars on the color–magnitude diagrams of young-age massive star clusters. Extended main-sequence turnoff as a common feature of Milky Way open clusters. Apparent age spreads in clusters and the role of stellar rotation. No evidence for significant age spreads in young massive LMC clusters. Dissecting the extended main-sequence turn-off of the young star cluster NGC 1850. Dynamical evidence for a range of ages being responsible for extended main-sequence turnoffs. Population parameters of intermediate-age star clusters in the Large Magellanic Cloud. Evidence for a bimodal distribution of rotational velocities for the single early B-type stars. A stellar rotation census of B stars: from ZAMS to TAMS. Stars caught in the braking stage in young Magellanic Cloud clusters. How stellar rotation shapes the colour–magnitude diagram of the massive intermediate-age star cluster NGC 1846. Tidal-locking-induced stellar rotation dichotomy in the open cluster NGC 2287? Astrophys. NGC 2818 and the role of stellar rotation. Extended main sequence turnoffs in open clusters as seen by Gaia-I. Different stellar rotations in the two main sequences of the young globular cluster NGC 1818: the first direct spectroscopic evidence. NGC 1866: first spectroscopic detection of fast-rotating stars in a young LMC cluster. The effect of stellar rotation on colour–magnitude diagrams: on the apparent presence of multiple populations in intermediate age stellar clusters. No evidence of chemical anomalies in the bimodal turnoff cluster NGC 1806 in the Large Magellanic Cloud. Mucciarelli, A., Dalessandro, E., Ferraro, F. Extended main-sequence turnoffs in the double cluster h and χ Persei: the complex role of stellar rotation. A survey of multiple sequences and Be stars in young clusters. Multiple stellar populations in Magellanic Cloud clusters-VI. Discovery of extended main-sequence turnoffs in four young massive clusters in the Magellanic Clouds. The double main sequence of the young cluster NGC 1755. Multiple stellar populations in Magellanic Cloud clusters-IV. An ordinary feature for intermediate age globulars in the LMC? Astron. Multiple stellar populations in Magellanic Cloud clusters. The atlas of multiple stellar populations. The Hubble Space Telescope UV Legacy Survey of Galactic globular clusters-IX. Lessons learned from the Milky Way globular clusters. Multiple populations in globular clusters. Observational Hertzsprung–Russell diagrams. Stellar evolution within and off the main sequence. Our findings shed new light on the origin of the bimodal mass, spin and magnetic-field distributions of main-sequence stars. This supports recent binary-formation models, and explains new velocity dispersion measurements for members of young star clusters. We also derive the approximate merger time of the individual stars of the blue main-sequence component, and find a strong early peak in the merger rate, with a lower-level merger activity prevailing for tens of millions of years. Our results imply that the cluster stars gain their mass in two different ways: by disk accretion leading to rapid rotation, contributing to the red main sequence, or by binary merger leading to slow rotation, populating the blue main sequence. We derive the masses of the blue main-sequence stars, and find that they follow a nearly flat mass function, which supports their unusual formation path. On the basis of their distribution in the colour–magnitude diagram, we show that stars of the blue main-sequence component can be understood as slow rotators originating from stellar mergers. Recent high-quality Hubble Space Telescope photometry shows that the main-sequence stars of young star clusters form two discrete components in the colour–magnitude diagram.
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