Evolution of long-lived globular cluster stars

Chantereau, William; Charbonnel, C.; Meynet, Georges

doi:10.1051/0004-6361/201628418

Cited by 47 publications

(75 citation statements)

References 92 publications

(115 reference statements)

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“…Finally, the correlation between the initial He and Na content given by the FRMS scenario and used by Chantereau et al (2016) provides a straightforward explanation to the lack of sodium-rich 2P AGB stars in GCs like NGC 6752 observations by Campbell et al 2013) due to the impact of the initial helium content on the stellar lifetime and evolution path in the Hertzsprung38Title : Stellar Clusters: Benchmarks for Stellar Physics and Galactic Evolution (EES 2015) Russel diagram. They also account for the finding of different sodium spreads that are observed along the AGB in the Galactic globular clusters of different ages and [Fe/H] values (Charbonnel and Chantereau, 2016;Wang et al, 2016).…”

Section: Consequences For Synthetic Globular Clustersmentioning

confidence: 90%

Section: Fast Rotating Massive Stars -Nucleosynthesismentioning

confidence: 99%

“…Additionally since helium is the main outcome of H-burning the abundance patterns are predicted to be correlated to various degrees with helium enrichment 7 . So far, the theoretical He enrichment is higher than allowed by observations and by isochrone fitting Chantereau et al, 2016) as discussed in details in § 7.et de hoc satis with the FRMS hypothesis? It may be too early to say (as for the AGB scenario), since the input physics of the FRMS models is also highly perfectible.…”

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confidence: 90%

“…5) can be directly used to determine the dilution ratio between the slow wind and interstellar material necessary to form 2P stars (e.g. Decressin et al 2007a;Lind et al 2009;Chantereau et al 2016).In summary, in the original FRMS models the C-N and O-Na anticorrelations as well as the Al increase appear naturally in the FRMS yields. An important increase of the rate of the reaction 24 Mg(p,γ) is however necessary to produce a Mg-Al anticorrelation.…”

mentioning

confidence: 99%

“…7.2 Impact of the initial helium content on the evolution of a low-mass star Numerous papers have been devoted to the study of the impact of the initial helium content of a star on its evolution (Iben and Faulkner, 1968;Hartwick and van den Berg, 1973;Lee, 1978;Sweigart and Gross, 1978;D'Antona et al, 2002D'Antona et al, , 2005Caloi, 2004, 2008;Salaris et al, 2006;Bertelli et al, 2008;Pietrinferni et al, 2009;D'Antona et al, 2010;Valcarce et al, 2012;Karakas, 2014;Dotter et al, 2015;Chantereau et al, 2015Chantereau et al, , 2016. We describe and illustrate the main points below, using predictions of the theoretical models of Chantereau et al (2015) Reimers (1975, with the η parameter equal to 0.5) up to the end of central He-burning and of Vassiliadis and Wood (1993) in the more advanced evolution phases.…”

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Multiple Stellar Populations and Their Evolution in Globular Clusters: A Nucleosynthesis Perspective

Charbonnel

2016

EAS Publications Series

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Abstract. This paper presents a review of the characteristics of the multiple stellar populations observed in globular clusters, and of their possible origin. The current theoretical issues and the many open questions are discussed. Importance of globular clusters for cosmology and for galactic physicsGlobular clusters (GC) are magnificent astronomical objects that provide insight to a broad variety of astronomical and cosmological questions. These compact systems that contain between several hundreds of thousands and a million stars are among the oldest structures in the Universe. They are unique relics, witnesses, and clocks of the formation, assembly, dynamics, and evolution of galaxies and of their substructures, from the early to the present-day Universe. They play a key role in hierarchical cosmology, and potentially also in the reionization of the Universe, and they provide fundamental benchmarks for stellar evolution theory. However, their formation, evolution, and survival in a galactic and cosmological context are far from being understood.Determining the age of the oldest GCs through isochrone fitting of their observed color-magnitude diagram (CMD) was crucial for cosmology until the beginning of the 21 st century, as it provided the best lower limit to the age of the Universe (e.g. Carney, 2001, and references therein). Meanwhile, a robust determination of the age of the Universe was made possible thanks to precise observations of the cosmic microwave background (CMB) by the Wilkinson Microwave Anisotropy Probe and Planck satellites. The age of the universe is now estimated (EES 2015) to be ∼ 13.8 according to flat Λ CMD model that accurately reproduces the observed temperature of the power spectrum of the CMB (Planck Collaboration, Ade et al., 2015). This agrees with the current estimate of the age of the oldest Galactic GCs that were among the first baryonic structures to form in galaxies about 13 Gyr ago (e.g. VandenBerg et al., 2013).Determining the absolute and relative ages of GCs is still very important today, for various reasons. This helps constraining the models of the formation of these systems in the more general context of the formation and early evolution of galaxies (e.g. Fall and Rees, 1985;Harris, 1991;Forbes et al., 1997; van den Bergh, 2011). Different scenarios make indeed different predictions for the age of the oldest GCs, as well as for the dispersion in age at a given metallicity (or rather [Fe/H]) and/or galactocentric distance. There is a wealth of literature on these questions, and we quote here only a few illustrative examples. Brodie and Strader (2006) argue that the most metal-poor GCs, which inhabit the haloes of spiral galaxies, were created in low-mass dark matter haloes at redshift higher than 10 (see also Bromm and Clarke 2002), and that metal-rich GCs formed during later mergers of gas-rich structures that build up the parent galaxies. On the other hand, cosmological N-body simulations and semi-analytic models of galaxy and GC formation accounting for the impo...

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Section: Consequences For Synthetic Globular Clustersmentioning

confidence: 90%

Section: Fast Rotating Massive Stars -Nucleosynthesismentioning

confidence: 99%

mentioning

confidence: 90%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Multiple Stellar Populations and Their Evolution in Globular Clusters: A Nucleosynthesis Perspective

Charbonnel

2016

EAS Publications Series

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The Physics of Star Cluster Formation and Evolution

Krause¹,

Offner²,

Charbonnel³

et al. 2020

Space Sci Rev

107

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Star clusters form in dense, hierarchically collapsing gas clouds. Bulk kinetic energy is transformed to turbulence with stars forming from cores fed by filaments. In the most compact regions, stellar feedback is least effective in removing the gas and stars may form very efficiently. These are also the regions where, in high-mass clusters, ejecta from some kind of high-mass stars are effectively captured during the formation phase of some of the low mass stars and effectively channeled into the latter to form multiple populations. Star formation epochs in star clusters are generally set by gas flows that determine the abundance of gas in the cluster. We argue that there is likely only one star formation epoch after which clusters remain essentially clear of gas by cluster winds. Collisional dynamics is important in this phase leading to core collapse, expansion and eventual dispersion of every cluster. We review recent developments in the field with a focus on theoretical work.

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Evolution of long-lived globular cluster stars

Chantereau¹,

Charbonnel²,

Meynet³

2017

A&A

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Context. Globular clusters host stars with chemical peculiarities. The associated helium enrichment is expected to affect the evolution of stars, in general, and of low-mass stars, and in particular the progenitors of white dwarfs (WDs). Aims. We investigate the effects of different initial helium contents on the properties of WDs such as their masses, compositions, and the time since their formation. Methods. We used the grid of stellar models that we presented in the first papers of this series, which were computed for low-mass, low-metallicity stars with different helium content at [Fe/H] = −1.75 up to the end of the thermally pulsing asymptotic giant branch (TP-AGB) phase. We determined an initial-to-final mass relation as a function of the initial helium mass fraction, where the final mass is determined at the end of the TP-AGB phase. We couple the results with different possible distributions of the initial helium content for low-mass stars in NGC 6752 to predict the properties of WDs in this cluster. Results. In a globular cluster at a given age, the He enrichment implies lower initial masses for stars at a given phase. Thus it leads to a decrease of the masses of WDs reaching the cooling sequence. In addition the He enrichment increases the total mass and number of WDs and eventually allows the presence of He white dwarf from single progenitors. Conclusions. The low He enrichment determined in most globular clusters with different methods results in negligible effects on the white dwarf properties. However, in the few globular clusters that display a high He enrichment, this may significantly affect the characteristics of the WDs. In NGC 2808 and ω Centauri the high He enrichment even leads to the formation of He WDs from single He-rich progenitors. Therefore investigating the white dwarf mass domain in globular clusters with a high He enrichment would provide an additional indirect way to measure and constrain the He enrichment degree.

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Evolution of long-lived globular cluster stars

Cited by 47 publications

References 92 publications

Multiple Stellar Populations and Their Evolution in Globular Clusters: A Nucleosynthesis Perspective

Multiple Stellar Populations and Their Evolution in Globular Clusters: A Nucleosynthesis Perspective

The Physics of Star Cluster Formation and Evolution

Evolution of long-lived globular cluster stars

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