Main sequence12/8/2022 ![]() Hectochelle: a multiobject optical echelle spectrograph for the MMT. Summary of the contents and survey properties. Membership determination of stars using proper motions in the region of the open cluster M 11. Discovery of extended main sequence turn offs in Galactic open clusters. NGC 2818 and the role of stellar rotation. Extended main sequence turnoffs in open clusters as seen by Gaia: I. Cluster kinematics and stellar rotation in NGC 419 with MUSE and adaptive optics. Reddening and polarimetric studies toward IC 1805. ![]() Spin alignment of stars in old open clusters. NGC 1866: first spectroscopic detection of fast-rotating stars in a young LMC cluster. A survey of multiple sequences and Be stars in young clusters. Multiple stellar populations in Magellanic Cloud clusters-VI. in The Observation and Analysis of Stellar Photospheres 3rd edn 458–504 (Cambridge Univ. The Gaia–ESO large public spectroscopic survey. The Gaia–ESO public spectroscopic survey. The Gaia–ESO survey: CNO abundances in the open clusters Trumpler 20, NGC 4815, and NGC 6705. The Gaia–ESO Survey: abundance ratios in the inner-disk open clusters Trumpler 20, NGC 4815, NGC 6705. ![]() The Gaia–ESO Survey: stellar content and elemental abundances in the massive cluster NGC 6705. New photometry and surface density profiles. Comprehensive abundance analysis of red giants in the open clusters NGC 2527, 2682, 2482, 2539, 2335, 22. Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682). On the formation of multiple stellar populations in globular clusters. The effect of stellar rotation on colour–magnitude diagrams: on the apparent presence of multiple populations in intermediate age stellar clusters. NGC 1846 and its wide main-sequence turnoff. Population parameters of intermediate-age star clusters in the Large Magellanic Cloud. The age and age spread of the Praesepe and Hyades clusters: a consistent, ~800 Myr picture from rotating stellar models. The first evidence of an extended main sequence turn-off in a young cluster: NGC 1856. Multiple stellar populations in Magellanic Cloud clusters-III. The exclusion of a significant range of ages in a massive star cluster. Not-so-simple stellar populations in the intermediate-age Large Magellanic Cloud star clusters NGC 1831 and NGC 1868. An extended main-sequence turn-off in the Small Magellanic Cloud star cluster NGC 411. New insights from extended main-sequence turnoff in seven star clusters. A double main-sequence turn-off in the rich star cluster NGC 1846 in the Large Magellanic Cloud. ![]() Multiple stellar populations in globular clusters. Our synthetic cluster simulation further demonstrates how stellar rotation affects the colours of cluster members, suggesting that the colour spread observed in populous clusters can be understood in the context of stellar evolution without introducing multiple stellar populations.īastian, N. Monte Carlo simulations infer that cluster members have highly aligned spin axes and a broad distribution of equatorial velocities biased towards high velocities. Cluster members display a broad V eqsin i distribution, and fast rotators, including Be stars, have redder colours than slow rotators. Here, we report the distribution of projected rotational velocities ( V eqsin i) of stars in the Galactic open cluster M11, measured by Fourier transform analysis. However, its effectiveness has not yet been proven due to the lack of direct measurements of rotational velocities. Another approach to explain this feature is to introduce the effect of stellar rotation 11. A sequential evolution of multiple generations of stars formed over 100–200 Myr is a natural explanation of this colour spread 10. Star clusters have long been considered to comprise a simple stellar population, but this paradigm is being challenged, since in addition to multiple populations in Galactic globular clusters 1, a number of younger star clusters exhibit a significant colour spread at the main sequence turn-off 2, 3, 4, 5, 6, 7, 8, 9. ![]()
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