Dynamical Implications of Multiple Stellar Populations

Details Dynamical Implications of Multiple Stellar Populations Dynamical Implications of Multiple Stellar Populations

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd..14e..11s&link_type=abstract

Modelling Dense Stellar Systems, 26th meeting of the IAU, Joint Discussion 14, 22-23 August 2006, Prague, Czech Republic, JD14,

Computer Science

Scientific paper

Globular clusters are usually thought of as a simple population of stars that were formed in a single burst from a cloud of uniform composition. However, such a model is inconsistent with the detailed observations of abundances in globular cluster stars. Almost all clusters seem to have a constant value of iron or iron peak elements in their stars. However, every cluster that has been carefully studied shows star-to-star variation of lighter metals (C, N, O, Al, Mg, etc.) and possibly also helium for stars in all regions of the HR diagram. One possible mechanism to explain these variations is the self-enrichment scenario. This scenario takes a variety of forms, but always involves more than one star formation episode in the cluster. Dynamical models of star clusters have, to date, always assumed that reasonable 'initial conditions' are a coeval population of stars in dynamical equilibrium. These models tend to reproduce cluster observations well, but are inconsistent with the self-enrichment scenario. In this talk, I will explore the dynamical effects of having two star formation episodes in star clusters. In particular, I will explore models based on the assumption that the self-enrichment comes from an early generation of AGB stars. I will compare our results to standard, single-burst cluster models and discuss any observational implications.

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