Fast rotating massive stars and the origin of the abundance patterns in galactic globular clusters

By T. Decressin, G. Meynet, C. Charbonnel, N. Prantzos, S. Ekström. 2006

540 citations recorded by the source corpus.

Aims. We propose the Wind of Fast Rotating Massive Stars scenario to explain the origin of the abundance anomalies observed in globular clusters. Methods. We compute and present models of fast rotating stars with initial masses between 20 and 120 $M_\odot$ for an initial metallicity Z  = 0.0005 (${\rm [Fe/H]}\simeq-1.5$). We discuss the nucleosynthesis in the H-burning core of these objects and present the chemical composition of their ejecta. We consider the impact of uncertainties in the relevant nuclear reaction rates. Results. Fast rotating stars reach critical velocity at the beginning of their evolution and remain near the critical limit during the rest of the main sequence and part of the He-burning phase. As a consequence they lose large amounts of material through a mechanical wind which probably leads to the formation of a slow outflowing disk. The material in this slow wind is enriched in H-burning products and presents abundance patterns similar to the chemical anomalies observed in globular cluster stars. In particular, the C, N, O, Na and Li variations are well reproduced by our model. However the rate of the $\rm{}^{24}\kern-0.6ptMg$$(p,\gamma)$ has to be increased by a factor 1000 around 50 $\times$ 10 6  K in order to reproduce the amplitude of the observed Mg-Al anticorrelation. We discuss how the long-lived low-mass stars currently observed in globular clusters could have formed out of the slow wind material ejected by massive stars.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d4291a0932b577636bc9553d058c6fa7b71a885e

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In Astronomy and Astrophysics

1. R. Gratton
2. E. Carretta
3. A. Bragaglia
4. Jay Anderson
5. Aaron Dotter
6. F. D’Antona
7. G. Piotto
8. Martin Asplund

In Instrumentation

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

Citations in the corpus

• Quantifying the uncertainties of chemical evolution studies II. Stellar yields (2010, background): “Also, one must be aware that, in order to reproduce the Mg-Al anticorre- lation observed in globular clusters stars, Decressin et al. (2007) varied the rate of the nuclear reaction24Mg(p, γ)25Al by orders of magnitude outside of the published uncertainties.”
• MULTIPLE STELLAR POPULATIONS IN 47 Tucanae (2011, background): “…Galactic GCs (see Gratton et al. 2004 for a review), possibly in combination with accretion onto low-mass stars of ejecta from either intermediate-mass stars (D’Antona et al. 1983; Renzini 1983), fast-rotating massive stars (e.g., Decressin et al. 2007), or massive binaries (De Mink et al. 2009).”
• CHEMICAL ABUNDANCES FOR 855 GIANTS IN THE GLOBULAR CLUSTER OMEGA CENTAURI (NGC 5139) (2010, background): “…mechanisms are: (1) hot bottom burning in >5 M AGB stars (e.g., Ventura & D’Antona 2009; Karakas 2010), (2) hydrogen shell burning in now extinct but slightly more massive RGB stars (Denissenkov & Weiss 2004), and (3) core hydrogen burning in rapidly rotating massive stars (Decressin et al. 2007).”
• THE AGES OF 55 GLOBULAR CLUSTERS AS DETERMINED USING AN IMPROVED METHOD ALONG WITH COLOR–MAGNITUDE DIAGRAM CONSTRAINTS, AND THEIR IMPLICATIONS FOR BROADER ISSUES (2013, background): “…review by Gratton, Carretta, & Bragaglia (2012, also see Renzini 2008), current models for the AGB phase and for rapidly rotating massive stars (Decressin et al. 2007, and references therein) are not able to reproduce the observed abundance patterns in a fully satisfactory and consistent way.”
• Massive AGB models of low metallicity: the implications for the self-enrichment scenario in metal-poor globular clusters (2009, background): “…AGBs (Cottrell & Da Costa 1981; Ventura et al. 2001) or those from fast rotating massive stars (Prantzos & Charbonnel 2006) have been proposed as progenitors of the SG; the latter scenario is described in detail in Decressin et al. (2007) and references therein; here we follow the first hypothesis.”
• The Hubble Space Telescope UV Legacy Survey of Galactic globular clusters – IX. The Atlas of multiple stellar populations (2016, background): “It is indeed commonly believed that the multiple stellar populations phenomenon in GCs is the result of multiple events of star formation where 2G stars form out of material processed by 1G stars (e.g., Decressin et al. 2007,Paper V, D’Antona et al. 2016 and references therein).”
• Evolution towards the critical limit and the origin of Be stars (2007, background): “…either triggered by rotational ejection or through the enhancement of the CNO content of the outer layers, have (if realized) important consequences on the evolution of the first stellar generations as well as on their nucleosynthesis (Ekström et al. 2006; Hirschi 2007; Decressin et al. 2007).”
• Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog (2019, background): “In particular, studies of MPs can place important constraints on various cluster processes, especially those occurring during the earliest evolutionary phases of clusters (e.g., Ventura et al. 2001; Decressin et al. 2007; de Mink et al. 2009; Denissenkov & Hartwick 2014; Gieles et al. 2018).”
• 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).”
• The fraction of second generation stars in globular clusters from the analysis of the horizontal branch (2008, background): “…is the result of the dilution of pristine cluster matter (Y=0.24) with highly Y enriched matter (Y >∼ 0.34), as envisaged in many formation scenarios (Decressin et al. 2007; Ventura & D’Antona 2008b; D’Ercole et al. 2008), not necessarily the main chemical anomaly indicators will assume values…”
• Formation and dynamical evolution of multiple stellar generations in globular clusters (2008, methodology): “…Prantzos & Charbonnel 2006; D’Antona et al. 2007; Decressin et al. 2007b), or the system evolves at constant mass and the IMF is highly anomalous (D’Antona & Caloi 2004; Decressin et al. 2007b, see also Downing & Sills (2007) for a dynamical study) and contains a significant number of FG polluters.”
• Abundance patterns of multiple populations in globular clusters: a chemical evolution model based on yields from AGB ejecta (2010, background): “In fact, no other source can be able to deal, at the same time, with the reproduction of the Mg–poor, Al–rich stars (Decressin et al. 2007), and with the extreme but homogeneous helium content that is necessary to reproduce the triple main sequence (D’Ercole et al. 2008; D’Antona & Caloi 2008;…”
• PRE-SUPERNOVA EVOLUTION OF ROTATING SOLAR METALLICITY STARS IN THE MASS RANGE 13–120 M☉ AND THEIR EXPLOSIVE YIELDS (2012, methodology): “…grids of rotating massive stars – 4 – have been computed and discussed by Meynet & Maeder (2000, 2003); Hirschi et al. (2004); Meynet & Maeder (2005); Decressin et al. (2007); Ekström et al. (2008); Ekström et al. (2012) and Heger et al. (2000); Heger & Langer (2000); Heger et al. (2005); Yoon…”
• The second and third parameters of the horizontal branch in globular clusters (2010, background): “…O and Mg, we do not yet have a satisfactory detailed model, and even its astrophysical basis is currently debated (either fast rotating massive stars or massive AGB stars, experiencing hot bottom burning, or massive binaries: see Decressin et al. 2007; Ventura et al. 2001; De Mink et al. 2009).”
• Na-O anticorrelation and HB - VIII. Proton-capture elements and metallicities in 17 globular clusters from UVES spectra (2009, methodology): “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).”
• THE ACS SURVEY OF GALACTIC GLOBULAR CLUSTERS. IX. HORIZONTAL BRANCH MORPHOLOGY AND THE SECOND PARAMETER PHENOMENON (2009, background): “…models of chemical enrichment in GCs predict that the abundance variations from the primordial values should be accompanied by an increase in He, whether the source of the enrichment is massive stars (Decressin et al. 2007) or intermediate-mass asymptotic giant branch stars (D’Antona et al. 2002).”
• Properties of stellar generations in globular clusters and relations with global parameters (2010, background): “The most popular candidates are either intermediate-mass AGB stars (e.g., D’Antona & Ventura 2007) or very massive, rotating stars (FRMS, e.g., Decressin et al. 2007)1.”