The chemical evolution of globular clusters - II. Metals and fluorine

P Sanchez-Blazquez, A Marcolini, Brad Gibson, Amanda Karakas, Kate Pilkington, F Calura

Research output: Contribution to journalArticleResearchpeer-review

7 Citations (Scopus)


n the first paper in this series, we proposed a new framework in which to model the chemical evolution of globular clusters. This model, is predicated upon the as- sumption that clusters form within an interstellar medium enriched locally by the ejecta of a single Type Ia supernova and varying numbers of asymptotic giant branch stars, superimposed on an ambient medium pre-enriched by low-metallicity Type II supernovae. Paper I was concerned with the application of this model to the observed abundances of several reactive elements and so-called non-metals for three classical intermediate-metallicity clusters, with the hallmark of the work being the success- ful recovery of many of their well-known elemental and isotopic abundance anomalies. Here, we expand upon our initial analysis by (a) applying the model to a much broader range of metallicities (from the factor of three explored in Paper I, to now, a factor of a??50; i.e., essentially, the full range of Galactic globular cluster abundances, and (b) incorporating a broader suite of chemical species, including a number of iron- peak isotopes, heavier I?-elements, and fluorine. While allowing for an appropriate fine tuning of the model input parameters, most empirical globular cluster abundance trends are reproduced, our model would suggest the need for a higher production of calcium, silicon, and copper in low-metallicity (or so-called a??prompta??) Type Ia su- pernovae than predicted in current stellar models in order to reproduce the observed trends in NGC 6752, and a factor of two reduction in carbon production from asymp- totic giant branch stars to explain the observed trends between carbon and nitrogen. Observations of heavy-element isotopes produced primarily by Type Ia supernovae, including those of titanium, iron, and nickel, could support/refute unequivocally our proposed framework, although currently the feasibility of the proposed observations is well beyond current instrumental capabilities. Hydrodynamical simulations would be necessary to study its viability from a dynamical point of view
Original languageEnglish
Pages (from-to)1376 - 1389
Number of pages14
JournalMonthly Notices of the Royal Astronomical Society
Issue number2
Publication statusPublished - 2012

Cite this