Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 395, Issue 2, Pages 719-735Publisher
WILEY-BLACKWELL PUBLISHING, INC
DOI: 10.1111/j.1365-2966.2009.14591.x
Keywords
nuclear reactions, nucleosynthesis, abundances; stars: abundances; stars: AGB and post-AGB; stars: chemically peculiar; globular clusters: individual: NGC 6752, NGC 6205, NGC 2808
Categories
Funding
- Science & Technology Facilities Council [ST/F002432/1]
- Australian Research Council's Discovery [DP0664105]
- Marie Curie Intra-European Fellowship
- 6th European Community Framework Programme
- Australian Research Council [DP0664105] Funding Source: Australian Research Council
- STFC [ST/F002432/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/F002432/1] Funding Source: researchfish
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We propose a new chemical evolution model aimed at explaining the chemical properties of globular clusters (GCs) stars. Our model depends upon the existence of (i) a peculiar Wre-enrichment phase in the GC's parent galaxy associated with very low-metallicity Type II supernovae (SNe II) and (ii) localized inhomogeneous enrichment from a single Type Ia supernova (SN Ia) and intermediate-mass (4-7 M(circle dot)) asymptotic giant branch field stars. GC formation is then assumed to take place within this chemically peculiar region. Thus, in our model the first low-mass GC stars to form are those with peculiar abundances (i. e. O-depleted and Na-enhanced), while 'normal' stars (i. e. O-rich and Na-depleted) are formed in a second stage when self-pollution from SNe II occurs and the peculiar pollution from the previous phase is dispersed. In this study, we focus on three different GCs: NGC 6752, 6205 (M 13) and 2808. We demonstrate that, within this framework, a model can be constructed which is consistent with (i) the elemental abundance anticorrelations, (ii) isotopic abundance patterns and (iii) the extreme [O/Fe] values observed in NGC 2808 and M 13, without violating the global constraints of approximately unimodal [Fe/H] and C+N+O.
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