Other
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd..14e...2d&link_type=abstract
Modelling Dense Stellar Systems, 26th meeting of the IAU, Joint Discussion 14, 22-23 August 2006, Prague, Czech Republic, JD14,
Other
Scientific paper
Until a few years ago, the common paradigm for the formation of Globular Clusters (GCs) was that they constitute a `simple stellar population' in which all the stars were formed from a chemically homogeneous cluster medium within a relatively short interval of time, at the beginning of the galactic life. Consequently, the main relation between stellar modelling and dynamics were, on the one side, the occurrence of mass loss from massive stars and the consequent problems of survival of the cluster as such; on the other side, the dynamic evolution of the different populations characterized by different stellar mass (the massive black holes (BH) and neutron star (NS) remnants, the massive white dwarfs (WDs) and the blue stragglers (BS) population. In recent years, spectroscopic observations of turnoff cluster stars has forced recognition that chemical anomalies are a common feature of GCs, and not simply a feature of individual stellar evolution. This has provoked a revolution in the simple view of GC formation, and it is now well accepted that at least two different stellar components are common in most GCs, and even three in some of them. It will be shown that the two main components are almost unequivocally identified with 1) the first stellar generation, which gave origin to stars of all masses; 2) a second generation, born from the ejecta of the most massive asymptotic giant branch stars of the first generation, in the first 100 or 200 million years from the first burst of star formation. A `third' population is present only in some GCs, and is more difficult to be understood. It is characterized by stars having a huge helium content (Y~0.4, if stellar modelling is reasonable) and extreme chemical anomalies in the proton capture elements (Na, O, Al). The status of understanding of the GC properties, based on our most recent models of stellar evolution, is discussed, stressing that dynamical modelling of the early stages of GC formation is now required for a full understanding of the problem.
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