Formation and dynamical evolution of multiple stellar generations in globular clusters

Abstract

We study the formation and dynamical evolution of clusters with multiple stellar generations. Observational studies have found that some globular clusters host a population of second generation (SG) stars which show chemical anomalies and must have formed from gas containing matter processed in the envelopes of first generation (FG) cluster stars. We study the SG formation process by means of one‐dimensional (1D) hydrodynamical simulations, starting from a FG already in place and assuming that the SG is formed by the gas ejected by the asymptotic giant branch (AGB) stars. This gas collects in a cooling flow into the cluster core, where it forms SG stars. The SG subsystem emerging from this process is initially strongly concentrated in the cluster innermost regions and its structural properties are largely independent of the FG initial properties. We also present the results of 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 then study the two‐population cluster dynamical evolution and mass loss. In our simulations, 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 supernova (SN) ejecta. The SG population, initially concentrated in the innermost cluster regions, is largely unscathed by this early mass loss, and this early evolution leads to values of the number ratio of SG to FG stars consistent with observations. We also demonstrate possible evolutionary routes leading to the loss of most of the FG population, leaving an SG‐dominated cluster. As the cluster evolves and the two populations mix, the local ratio of SG to FG stars, initially a decreasing function of radius, tends to a constant value in the inner parts of the cluster. Until mixing is complete, the radial profile of this number ratio is characterized by a flat inner part and a declining portion in the outer cluster regions.

The morphology of the sub-giant branch and red clump reveal no sign of age spreads in intermediate-age clusters

“…Longmore et al 2014). Globular clusters, on the other hand, host chemical abundance anomalies within their stellar populations (e.g., Gratton et al 2012), and while age spreads cannot be discerned at these old ages, some scenarios to explain the anomalies invoke multiple star-forming epochs, spanning tens to hundreds of Myr (e.g., D'Ercole et al 2008;Conroy & Spergel 2011), although other scenarios have little or no age spreads (e.g., Krause et al 2013;Bastian et al 2013b). …”

G2C2 – IV. A novel approach to study the radial distributions of multiple populations in Galactic globular clusters

“…However, it may be possible to constrain these models via their effects on the radial distribution of polluted stars, i.e, the first and later generations. In general, E-mail: Joachimvanderbeke@gmail.com we expect that more enriched stars will tend to reside closer to the cluster centres, as the gas needed to fuel star formation tends to sink to the cluster core (e.g., D'Ercole et al 2008). In the early disk accretion model, the protostellar disks accrete material as they travel through the cluster and therefore one expects a somewhat broader distribution.…”

NGC 6362: The Least Massive Globular Cluster With Chemically Distinct Multiple Populations*

“…Within this general framework, four main scenarios have been proposed, differing mainly in the nature of the polluters: (i) asymptotic giant branch stars (D'Ercole et al 2008), (ii) fastrotating massive stars (Decressin et al 2007), (iii) interacting massive binary stars (De Mink et al 2009), and (iv) supermassive stars (Denissenkov & Hartwick 2014;Denissenkov et al 2015). An alternative scenario that does not require an age difference between first-and secondgeneration stars is the so-called early disk accretion scenario (Bastian et al 2013).…”