The rotation of selected globular clusters and the differential rotation of M3 in multiple populations from the SDSS-IV APOGEE-2 survey

Szigeti, László; Mészáros, Szabolcs; Szabó, Gyula; Fernández-Trincado, José G.; Cohen, Roger E.

doi:10.1093/mnras/stab1007

Cited by 12 publications

(13 citation statements)

References 71 publications

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“…To verify a direct connection with the formation process it is necessary to check the rotation of the 1P and 2P separately, to identify a differential rotation between the two populations. This has been done for few clusters, however, since the analysed clusters show significantly different behaviours, no firm conclusion has been yet achieved (Milone et al 2018;Cordoni et al 2020a,b;Szigeti et al 2021). Additionally, the strong correlation existing between cluster mass and rotation makes it difficult to disentangle between the relevance of these two properties with respect to the 2P origin.…”

Section: Discussion a N D C O N C L U S I O N Smentioning

confidence: 97%

“…Centrally concentrated 2P stars have been indeed observed in a number of clusters (see e.g. Norris & Freeman 1979;Milone et al 2012a;Richer et al 2013;Cordero et al 2014Cordero et al , 2017Bellini et al 2015;Dalessandro et al 2019;Kamann et al 2020;Dondoglio et al 2021;Szigeti et al 2021). The observed differences are milder for more dynamically evolved systems (Dalessandro et al 2019).…”

Section: Introductionmentioning

confidence: 91%

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Linking globular cluster structural parameters and their evolution: multiple stellar populations

Mastrobuono-Battisti

Perets

2021

Monthly Notices of the Royal Astronomical Society

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Globular clusters (GCs) are known to host multiple stellar populations showing chemical anomalies in the content of light elements. The origin of such anomalies observed in Galactic GCs is still debated. Here we analyse data compiled from the Hubble Space Telescope, ground-based surveys and Gaia DR2 and explore relationships between the structural properties of GCs and the fraction of second population (2P) stars. Given the correlations we find, we conclude that the main factor driving the formation/evolution of 2P stars is the cluster mass. The existing strong correlations between the 2P fraction and the rotational velocity and concentration parameter could derive from their correlation with the cluster mass. Furthermore, we observe that increasing cluster escape velocity corresponds to higher 2P fractions. Each of the correlations found is bimodal, with a different behaviour detected for low and high mass (or escape velocity) clusters. These correlations could be consistent with an initial formation of more centrally concentrated 2P stars in deeper cluster potentials, followed by a long-term tidal stripping of stars from clusters outskirts. The latter are dominated by the more extended distributed first population (1P) stars, and therefore stronger tidal stripping would preferentially deplete the 1P population, raising the cluster 2P fraction. This also suggests a tighter distribution of initial 2P fractions than observed today. In addition, higher escape velocities allow better retention of low-velocity material ejected from 1P stars, providing an alternative/additional origin for the observed differences and the distributions of 2P fractions amongst GCs.

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Section: Discussion a N D C O N C L U S I O N Smentioning

confidence: 97%

Section: Introductionmentioning

confidence: 91%

Linking globular cluster structural parameters and their evolution: multiple stellar populations

Mastrobuono-Battisti

Perets

2021

Monthly Notices of the Royal Astronomical Society

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“…We have shown, for the first time, that the young SMC SCs can have internal rotation just after their formation from their natal GMCs. Although this is one key prediction from the present simulation, almost all recent studies of SCs have investigated the internal kinematics of stars in the old Galactic GCs (e.g., Barth et al 2020;Kamann et al 2020;Szigeti et al 2021). Accordingly, it is not possible for the present study to discuss the physical origin of the simulated rotational kinematics of some SCs based on the latest observations of SCs in the SMC.…”

Section: Internal Rotation Of Young Scs In the Smcmentioning

confidence: 84%

Star cluster formation from giant molecular clouds in the Small Magellanic Cloud about 2 Gyr ago: their origin, structures, and kinematics

Williams,

Bekki,

McKenzie

2021

Preprint

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Recent observations have found that the age distribution of star clusters (SCs) in the Small Magellanic Cloud (SMC) shows a sharp peak around 2 Gyr ago. However, it is theoretically unclear what physical processes are responsible for such sudden formation of SCs in the SMC. Here we investigate whether massive SCs with initial masses more than 10 5 M can be formed during tidal interaction of the SMC with the Large Magellanic Cloud (LMC) about 2 Gyr ago, based on our new simulations, which include molecular hydrogen formation on dust grains and SC formation within giant molecular clouds (GMCs). We find that the formation of GMCs with masses more than 10 5 M can be dramatically enhanced due to the tidal force of the LMC-SMC interaction. We also find that gravitationally bound massive SCs can be formed within these GMCs, though their mean stellar densities (10 4 M pc −3 ) are systematically lower than those of the genuine globular clusters (GCs). All simulated SCs have diffuse extended stellar envelopes that were formed from multiple merging of sub clusters within their natal GMCs. Furthermore, we find that some of the simulated SCs can have considerable global internal rotation and substructures surrounding them. Based on these simulation results, we discuss the origin of the observed diverse properties of SCs in the SMC and the physical roles of galaxy interaction in the formation of massive SCs from GMCs.

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“…Recently, Cordero et al (2017) and Kamann et al (2020) analyzed the rotational patterns of two GCs subpopulations and found that extreme SG stars (Na-enhanced and extremely O-depleted) are characterized by a larger rotational amplitude than intermediate SG ones (moderately Na-enhanced and O-depleted). In some cases, instead, no difference as been detected in the rotational patters of distinct populations (Milone et al 2020;Cordoni et al 2020a,b;Szigeti et al 2021). This rotational homogeneity between different populations could hint that these systems are dynamically evolved, where stars are already well kinematically mixed.…”

Section: Introductionmentioning

confidence: 98%

“…The observational study of the kinematics of multiple stellar populations is still in its early stages, but a few investigations have already revealed differences in the rotation amplitudes between stellar populations (Lee 2015(Lee , 2017(Lee , 2018Dalessandro et al 2021;Cordoni et al 2020a;Szigeti et al 2021), with the SG component rotating faster than the FG, with the exception of 𝜔 Cen where Bellini et al (2018) found opposite results. Recently, Cordero et al (2017) and Kamann et al (2020) analyzed the rotational patterns of two GCs subpopulations and found that extreme SG stars (Na-enhanced and extremely O-depleted) are characterized by a larger rotational amplitude than intermediate SG ones (moderately Na-enhanced and O-depleted).…”

Section: Introductionmentioning

confidence: 99%

The role of rotation on the formation of second generation stars in globular clusters

Lacchin

Calura²,

Vesperini

et al. 2022

Monthly Notices of the Royal Astronomical Society

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By means of 3D hydrodynamic simulations, we explore the effects of rotation in the formation of second-generation (SG) stars in globular clusters (GC). Our simulations follow the SG formation in a first-generation (FG) internally rotating GC; SG stars form out of FG asymptotic giant branch (AGB) ejecta and external pristine gas accreted by the system. We have explored two different initial rotational velocity profiles for the FG cluster and two different inclinations of the rotational axis with respect to the direction of motion of the external infalling gas, whose density has also been varied. For a low (10−24g cm−3) external gas density, a disk of SG helium-enhanced stars is formed. The SG is characterized by distinct chemo-dynamical phase space patterns: it shows a more rapid rotation than the FG with the helium-enhanced SG subsystem rotating more rapidly than the moderate helium-enhanced one. In models with high external gas density (10−23g cm−3), the inner SG disc is disrupted by the early arrival of external gas and only a small fraction of highly enhanced helium stars preserves the rotation acquired at birth. Variations in the inclination angle between the rotation axis and the direction of the infalling gas and the velocity profile can slightly alter the extent of the stellar disc and the rotational amplitude. The results of our simulations illustrate the complex link between dynamical and chemical properties of multiple populations and provide new elements for the interpretation of observational studies and future investigations of the dynamics of multiple-population GCs.

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The rotation of selected globular clusters and the differential rotation of M3 in multiple populations from the SDSS-IV APOGEE-2 survey

Cited by 12 publications

References 71 publications

Linking globular cluster structural parameters and their evolution: multiple stellar populations

Linking globular cluster structural parameters and their evolution: multiple stellar populations

Star cluster formation from giant molecular clouds in the Small Magellanic Cloud about 2 Gyr ago: their origin, structures, and kinematics

The role of rotation on the formation of second generation stars in globular clusters

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