<p> In this thesis we investigate the dynamical effect of a second generation of stellar formation in globular clusters in the context of the anomalous horizontal branch of NGC 2808. The horizontal branch of NGC 2808 is bifurcated in colour and exhibits an extended blue tail. This morphology can be explained if the blue tail stars have an enhanced helium content due to cluster self-enrichment. Specifically it has been proposed that NGC 2808 has experienced
two distinct generations of star formation. The first generation has a top-heavy IMF, enhanced in 3 - 5Mo stars, and would produce many AGB stars within the first 200 Myrs of its life. The second generation then forms out of the helium-rich ejecta of the AGB stars and goes on to produce the blue tail in the horizontal branch that is currently observed in NGC 2808.</p> <p> We use three types of simulations to investigate this scenario. For a control model we run a simulation with a Salpeter IMF and a single generation. We then run models with a top-heavy IMF and a single generation and models with a top-heavy IMF and two generations. In the two generation models we also investigate the effect of concentration by examining simulations with two different length scales.</p> <p> We find that the models with the top-heavy IMF and a single generation are subject to extensive mass-loss in their early phases due to the large number of intermediate-mass stars and are less strongly affected by two-body
relaxation than simulations with a Salpeter IMF. The models with two generations appear to be dynamically stable and long-lived objects, at least in their early stages. They seem to be observationally indistinguishable from single-generation clusters with Salpeter IMFs on the basis of their dynamics. The stellar populations of the two-generation clusters are found to have a much higher fraction of C-O white dwarfs than clusters with a Salpeter IMF. We find no evidence that these bodies will be preferentially scattered out of the system and they should remain part of the cluster until it dissolves after core collapse. The abundance of white dwarfs would provide an observational method of identifying two generation cluster candidates.</p> <p> Overall we find the two-generation scenario to be plausible on the basis of dynamics but due to the overabundance of white dwarfs produced by the top-heavy IMF and based on other studies of the chemistry of AGB stars we conclude that this scenario is unlikely to be the sole explanation for globular cluster self-enrichment.</p> / Thesis / Master of Science (MSc)
| Identifer | oai:union.ndltd.org:mcmaster.ca/oai:macsphere.mcmaster.ca:11375/21583 |
| Date | 07 1900 |
| Creators | Downing, Jonathan M. B. |
| Contributors | Sills, Alison, Physics and Astronomy |
| Source Sets | McMaster University |
| Language | en_US |
| Detected Language | English |
| Type | Thesis |
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