Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21333105v&link_type=abstract
American Astronomical Society, AAS Meeting #213, #331.05; Bulletin of the American Astronomical Society, Vol. 41, p.391
Astronomy and Astrophysics
Astronomy
Scientific paper
We present the results of hydrodynamical and N-body simulations aimed at studying the formation and dynamical evolution of multiple stellar generations in globular clusters.
By means of 1D hydrodynamical simulations, we study the formation of a second stellar generation (SG) from the gas ejected by AGB stars. This gas collects in a cooling flow into the cluster core, where it forms a SG subsystem strongly concentrated in the cluster innermost regions with structural properties largely independent of the initial properties of the first generation (FG) stars. We have also explored a model in which pristine gas contributes to the SG formation. In this model a very helium-rich SG population and one with a moderate helium enrichment form; the resulting SG bimodal helium distribution resembles that observed for SG stars in NGC 2808.
By means of N-body simulations, we study the two-population cluster dynamical evolution; our simulations show that a large fraction of FG stars are lost early in the cluster evolution due to the expansion and stripping of the cluster outer layers resulting from early mass loss associated with FG SN ejecta. The SG population is largely unscathed by this early mass loss, and this early evolution leads to values of the SG to FG number ratio consistent with observations. We also demonstrate possible evolutionary routes leading to the loss of most of the FG population, leaving an SG-dominated cluster. Until mixing of the two populations is complete, the radial profile of the SG to FG number ratio is characterized by a flat inner part and a declining portion in the outer cluster regions.
D'Antona Francesca
D'Ercole Annibale
McMillan Stephen L. W.
Recchi Simone
Vesperini Enrico
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