Predictions for Self-Pollution in Globular Cluster Stars

By P. Ventura, F. D’Antona, I. Mazzitelli, R. Gratton. 2001

330 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c1abd9bf4607b9cdb48af1c43987c15f211ace86

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In Astronomy and Astrophysics

1. R. Gratton
2. E. Carretta
3. A. Bragaglia
4. F. D’Antona
5. Jay Anderson
6. A. Renzini
7. G. Piotto
8. A. Milone

In Instrumentation

1. R. Gratton
2. F. D’Antona
3. E. Carretta
4. A. Bragaglia
5. A. Renzini
6. G. Piotto
7. Jay Anderson
8. A. Milone

Citations in the corpus

• Young Massive Star Clusters (2010, background): “…are rapidly rotating massive stars (Prantzos & Charbonnel 2006, Decressin et al. 2007) and massive (4–9 M⊙) Asymptotic Giant Branch (AGB) stars (Ventura et al. 2001, Karakas & Lattanzio 2007 In order to form the large fraction of SG stars suggested by observations (50% or more of the current…”
• Abundances of C, N, O in slightly evolved stars in the globular clusters NGC 6397, NGC 6752 and 47 Tuc (2004, background): “However, after initial successes (see e.g. Ventura et al. 2001), more recent models of metal-poor IM-AGB stars met serious problems in reproducing the O-Na anticorrelation and related phenomenology (Denissenkov & Herwig 2003; Fenner et al. 2004; Herwig 2004), and unveiled that not only Hot Bottom…”
• Formation and dynamical evolution of multiple stellar generations in globular clusters (2008, background): “…simple idea that the AGB winds are slow enough to be retained in the potential well of the cluster, and that these winds are processed through the hot CNO cycle by “Hot Bottom Burning” (Cameron & Fowler 1971; Sackmann & Boothroyd 1992) at the bottom of the convective envelope (Ventura et al. 2001).”
• Abundances in a Large Sample of Stars in M3 and M13 (2004, background): “The physical process responsible for these star-to-star element variations is still uncertain (see the reviews of Kraft 1994 and Pinsonneault 1997, as well as Cohen et al. 2002 and Ventura et al. 2001).”
• Abundance Variations within Globular Clusters (2004, methodology): “…CARRETTA formed within the cluster (the Cottrell & Da Costa scenario), or may have been accreted in appreciable fraction by existing stars with a well-developed radiative core (the accretion scenario: D’Antona, Gratton & Chieffi 1983; Cannon et al. 1998; Ventura et al. 2001; Thoul et al. 2002).”
• Intrinsic iron spread and a new metallicity scale for globular clusters (2009, background): “Star to star abundance variations in these elements are expected to also come with differences in the main outcome of the H burning, the He content (Gratton et al. 2009; Bragaglia et al. in preparation; Prantzos & Charbonnel 2006; Ventura et al. 2001).”
• Fast rotating massive stars and the origin of the abundance patterns in galactic globular clusters (2006, background): “However recent custommade stellar models (Ventura et al. 2001, 2002; Denissenkov & Herwig 2003; Karakas & Lattanzio 2003; Herwig 2004a,b; Ventura & D’Antona 2005a–c, 2006; Decressin et al., in preparation) pointed out very severe difficulties from the nucleosynthesis point of view which stem from…”
• Massive AGB models of low metallicity: the implications for the self-enrichment scenario in metal-poor globular clusters (2009, background): “…HBB, Blöcker & Schönberner 1991; D’Antona & Mazzitelli 1996), the products of which would be carried to the surface by the convective currents (Ventura et al. 2001): the medium in which this generation of stars evolved would thus show the signature of such nucleosynthesis, because the…”
• Massive binaries as the source of abundance anomalies in globular clusters (2009, background): “…sources of processed ejecta have been proposed: the slow winds ofmassive AGB stars, which enrich their convective envelopes with H-burning products (Ventura et al. 2001; D’Antona et al. 2002; Denissenkov & Herwig 2003) and fastrotating massive stars (we refer to these asspin stars), which are…”
• Na-O anticorrelation and HB - VIII. Proton-capture elements and metallicities in 17 globular clusters from UVES spectra (2009, background): “Candidate first-generation polluters are thermally pulsing, intermediatemass AGB stars undergoing hot bottom burning (see Ventura et al. 2001), or massive, rotating stars (see Decressin et al. 2007).”
• A Helium Spread among the Main-Sequence Stars in NGC 2808 (2005, methodology): “This is generally attributed to pollution from the winds of the massive AGBs (e.g. Cottrell & Da Costa 1981; D’Antona, Gratton, & Chieffi 1983; D’Antona 2003), whose convective envelopes are subject to hot bottom burning (HBB) (e.g. Ventura et al. 2001; Ventura, D’Antona, & Mazzitelli 2002).”
• The Chemical Composition Contrast between M3 and M13 Revisited: New Abundances for 28 Giant Stars in M3 (2003, background): “2162 stages (Cottrell & Da Costa 198l; Cannon et al. 1998; Ventura et al. 2001; Yong et al. 2003).”
• Spectroscopic and photometric evidence of two stellar populations in the Galactic globular cluster NGC 6121 (M 4) (2008, background): “…be primordial, i.e. they are derived from the chemical compositi n of the primordial site where the GC stars have been generated, or alternatively, that a second generation of stars has been formed from a medium enriched in some elements (e.g., the self enrichment model by Ventura et al. 2001).”
• Na-O Anticorrelation and HB. VII. The chemical composition of first and second-generation stars in 15 globular clusters from GIRAFFE spectra (2009, background): “We do not have a satisfactory model yet for the mechanism responsible of the Na-O anticorrelation, and even the astrophysical site is currently debated (fast-rotating massive starsvs massive AGB stars undergoing hot bottom burning: see Decressin et al. 2007; Ventura et al. 2001).”
• Full computation of massive AGB evolution. I. The large impact of convection on nucleosynthesis (2004, methodology): “In this case, to have an idea of the mean chemical composition of the ejecta of the star, we use the mass as abscissa instead of time (Ventura et al. 2001); the difference is relevant, because most of the mass is lost in correspondence of the maximum luminosity, in a time interval which is very…”
• The Double Subgiant Branch of NGC 1851: The Role of the CNO Abundance (2007, background): “Winds of intermediate-mass asymptotic giant branch (AGB) stars or winds of fast-rotating massive stars have been invoked as sources of the necessary heavy-element pollution (see, e.g., Ventura et al. 2001; Decressin et al. 2007; D’Antona & Ventura 2007 and references therein).”
• The two metallicity groups of the globular cluster M 22: a chemical perspective (2011, background): “However the debate on the possible polluters is still open (Ventura et al. 2001, D’Antona & Ventura 2007, Decressin et al. 2007).”