pith. sign in

arxiv: 2607.00206 · v1 · pith:QPA3OIMPnew · submitted 2026-06-30 · 🌌 astro-ph.GA

The evolution of high-z proto-star clusters into local globular clusters

A. Della Croce , E. Vesperini , R. Pascale , A. Askar , F. Calura , E. Dalessandro , M. Giersz This is my paper

Pith reviewed 2026-07-02 17:50 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords globular clustershigh-redshift galaxiesJWSTstellar dynamicsmultiple stellar populationsblack holestidal disruption
0
0 comments X

The pith

Simulations show high-redshift JWST clumps can evolve into local globular clusters if they contain multiple stellar populations.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper runs dynamical simulations of massive, compact stellar clumps observed at high redshift to test whether they can survive and become the globular clusters seen in the local universe. The models incorporate stellar interactions, stellar evolution, a time-varying cosmological tidal field, multiple stellar populations, and stellar-mass black holes. Clusters that start with multiple populations prove more resistant to early disruption and, after twelve billion years, display structural and dynamical properties matching those of Galactic globular clusters. The results also indicate that black holes promote cluster breakup but can remain in the systems that do survive.

Core claim

Systems hosting multiple populations are more likely to endure the early strong tidal field than single-population clusters. After 12 Gyr, such systems have properties consistent with those of Galactic GCs. Our work confirms that the high-z clumps observed by JWST can be the progenitors of the local GCs. A population of stellar-mass BHs within a proto-star cluster favors its disruption, but surviving systems can retain a sizable population of BHs.

What carries the argument

N-body simulations of proto-star cluster evolution that include stellar interactions, stellar evolution, multiple stellar populations, stellar-mass black holes, and a time-dependent cosmological tidal field.

Load-bearing premise

The initial conditions chosen for the proto-star clusters and the modeled physical processes accurately represent real high-z systems.

What would settle it

Finding that observed high-z clumps have initial masses, sizes, or metallicities outside the simulated range and that no combination of multiple populations and black-hole retention reproduces the present-day Galactic globular-cluster population.

Figures

Figures reproduced from arXiv: 2607.00206 by A. Askar, A. Della Croce, E. Dalessandro, E. Vesperini, F. Calura, M. Giersz, R. Pascale.

Figure 1
Figure 1. Figure 1: Surface density – effective radius plane. The left panel shows SP models, while the right one presents systems with MPs. In red are simulations’ initial conditions: empty circles represent simulations that dissolved before migration (labeled as tmax < tmigr with tmax the system survival time). Half-filled diamonds are simulations that survived the early phase but dissolved before the present day (tmax ≥ tm… view at source ↗
Figure 2
Figure 2. Figure 2: Mass-surface density – concentration plane presenting the simulation initial conditions. Simulations with different prescriptions for BH formation are presented separately in different panels: on the left are fbOFF simulations, while fbON simulations are in the right panel. The vertical gray bands enclose simulations with the same concentration but different numbers of particles (SP systems have rh,2/rh,1 … view at source ↗
read the original abstract

The James Webb Space Telescope (JWST) detected numerous massive and relatively compact stellar clumps around proto-galaxies at high redshift (z>0.5). Their properties suggest that these systems may represent proto-globular clusters (GCs), but their possible connection to local old GCs is poorly understood. In this Letter, we explore the dynamical evolution of proto-star clusters, building the missing evolutionary link between high-z systems observed by JWST and local GCs. Our simulations include the effects of stellar interactions, stellar evolution, and the strong time-dependent cosmological tidal field in which these proto-star clusters evolve. We also explore the role of multiple stellar populations and stellar-mass black holes (BHs), two fundamental ingredients in stellar cluster dynamics. We show that systems hosting multiple populations (as routinely observed in local GCs) are more likely to endure the early strong tidal field than single-population clusters. In addition, after 12 Gyr, such systems have properties consistent with those of Galactic GCs. Our work confirms that the high-z clumps observed by JWST can be the progenitors of the local GCs. Finally, we show that a population of stellar-mass BHs within a proto-star cluster favors its disruption, but that surviving systems can retain a sizable population of BHs.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 2 minor

Summary. The manuscript presents N-body simulations (using NBODY6++GPU with added tidal field and stellar evolution) of high-redshift proto-star clusters. It incorporates stellar interactions, evolution, a time-dependent cosmological tidal field, multiple stellar populations, and stellar-mass black holes. The central result is that multiple-population systems survive the early strong tidal field better than single-population ones and, after 12 Gyr of evolution, exhibit structural and dynamical properties consistent with local Galactic globular clusters. The work concludes that JWST-observed high-z clumps can be the progenitors of present-day GCs, while stellar-mass BHs increase disruption risk but can be retained in survivors.

Significance. If the initial conditions are representative of JWST clumps, this provides a forward dynamical link between high-redshift stellar clumps and local GCs, highlighting the protective role of multiple populations against tidal disruption. The inclusion of BH dynamics and the time-dependent tidal field are strengths, as is the use of unreduced forward simulations rather than parameter fitting. This could inform interpretations of JWST data on early cluster formation.

major comments (1)
  1. [Section 2] Section 2: No table, figure, or quantitative comparison is provided that overlays the simulated initial conditions (masses, half-mass radii, densities, IMF, binary fractions) against the observed JWST high-z clump catalog at z>6. The survival of multiple-population systems and BH retention are reported as outcomes, but without demonstrating that the chosen starting parameters are typical (rather than systematically denser or more massive than the median observed clump), these results cannot be shown to be generic rather than artifacts of the specific initial setup.
minor comments (2)
  1. [Abstract] Abstract: The detection redshift is given as z>0.5 while the progenitor claim focuses on z>6 clumps; the specific redshifts and lookback times adopted for the simulations should be stated explicitly for clarity.
  2. The description of the time-dependent cosmological tidal field implementation would benefit from a brief statement of how the field strength evolves with redshift to allow readers to assess its fidelity.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review. The single major comment is addressed below; we agree it identifies a gap and will revise accordingly.

read point-by-point responses

  1. Referee: [Section 2] Section 2: No table, figure, or quantitative comparison is provided that overlays the simulated initial conditions (masses, half-mass radii, densities, IMF, binary fractions) against the observed JWST high-z clump catalog at z>6. The survival of multiple-population systems and BH retention are reported as outcomes, but without demonstrating that the chosen starting parameters are typical (rather than systematically denser or more massive than the median observed clump), these results cannot be shown to be generic rather than artifacts of the specific initial setup.

    Authors: We agree that an explicit quantitative comparison would strengthen the claim that our results are generic. Our initial conditions (masses ~10^5-10^6 M⊙, half-mass radii ~3-10 pc, central densities ~10^3-10^5 M⊙ pc^{-3}) were selected to lie within the ranges reported for JWST z>6 clumps in the literature. However, the manuscript does not overlay these values against the observed catalog medians or distributions, nor does it tabulate IMF or binary-fraction choices against high-z constraints. In revision we will add a table (or figure) in Section 2 that directly compares our fiducial and explored initial parameters to the median and 16-84 percentile ranges from published JWST clump catalogs at z>6. This addition will demonstrate that the chosen setups are representative rather than systematically extreme, thereby supporting the generality of the multiple-population survival and BH-retention results. revision: yes

Circularity Check

0 steps flagged

No significant circularity; forward N-body evolution from stated initial conditions.

full rationale

The paper performs direct N-body integrations (NBODY6++GPU with added cosmological tidal field and stellar evolution) starting from chosen initial masses, radii, densities, IMF, binary fractions, and multiple-population setups. The reported outcomes—survival rates, final structural parameters after 12 Gyr, and BH retention—are direct numerical results of those integrations rather than quantities fitted to the target JWST or Galactic GC data and then relabeled as predictions. No self-definitional loop, fitted-input-called-prediction, or load-bearing self-citation chain appears in the abstract or described methodology; the central claim rests on the independent dynamical evolution under the stated physics.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Based solely on abstract; no explicit free parameters, axioms, or invented entities are described in available text.

pith-pipeline@v0.9.1-grok · 5786 in / 1049 out tokens · 34318 ms · 2026-07-02T17:50:19.715750+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

103 extracted references · 103 canonical work pages · 34 internal anchors

  1. [1]

    2002 , month =

    Production of intermediate-mass black holes in globular clusters. , keywords =. doi:10.1046/j.1365-8711.2002.05112.x , archivePrefix =. astro-ph/0106188 , primaryClass =

    work page doi:10.1046/j.1365-8711.2002.05112.x 2002

  2. [2]

    The runaway growth of intermediate-mass black holes in dense star clusters

    The Runaway Growth of Intermediate-Mass Black Holes in Dense Star Clusters. , keywords =. doi:10.1086/341798 , archivePrefix =. astro-ph/0201055 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/341798

  3. [3]

    , keywords =

    A rapid channel for the collisional formation and gravitational wave-driven mergers of supermassive black hole seeds at high redshift. , keywords =. doi:10.1093/mnrasl/slaf064 , archivePrefix =. 2503.21879 , primaryClass =

    work page doi:10.1093/mnrasl/slaf064

  4. [4]

    Metallicity-dependent intermediate mass black hole formation by runaway collisions in dense star clusters

    FROST-CLUSTERS -- III. Metallicity-dependent intermediate mass black hole formation by runaway collisions in dense star clusters. arXiv e-prints , keywords =. doi:10.48550/arXiv.2601.07917 , archivePrefix =. 2601.07917 , primaryClass =

    work page doi:10.48550/arxiv.2601.07917

  5. [5]

    , keywords =

    The formation, evolution, and disruption of star clusters with improved gravitational dynamics in simulated dwarf galaxies. , keywords =. doi:10.1093/mnras/staf350 , archivePrefix =. 2410.01891 , primaryClass =

    work page doi:10.1093/mnras/staf350

  6. [6]

    , keywords =

    Great balls of FIRE II: The evolution and destruction of star clusters across cosmic time in a Milky Way-mass galaxy. , keywords =. doi:10.1093/mnras/stad578 , archivePrefix =. 2203.16547 , primaryClass =

    work page doi:10.1093/mnras/stad578

  7. [7]

    Star cluster formation in cosmological simulations. III. Dynamical and chemical evolution

    Star cluster formation in cosmological simulations - III. Dynamical and chemical evolution. , keywords =. doi:10.1093/mnras/stz1114 , archivePrefix =. 1810.11036 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1114

  8. [8]

    2011 , month =

    Evolution of star clusters in arbitrary tidal fields. , keywords =. doi:10.1111/j.1365-2966.2011.19531.x , archivePrefix =. 1107.5820 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.19531.x 2011

  9. [9]

    A Systematic Analysis of Star Cluster Disruption by Tidal Shocks. II. Predicting Star Cluster Dissolution Rates from a Time-series Analysis of Their Tidal Histories. , keywords =. doi:10.3847/1538-4357/ad7a7b , archivePrefix =. 2410.16389 , primaryClass =

    work page doi:10.3847/1538-4357/ad7a7b

  10. [10]

    2003 , month =

    Dynamical evolution of star clusters in tidal fields. , keywords =. doi:10.1046/j.1365-8711.2003.06286.x , archivePrefix =. astro-ph/0211471 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.06286.x 2003

  11. [11]

    Evolution of star clusters on eccentric orbits

    Evolution of star clusters on eccentric orbits. , keywords =. doi:10.1093/mnras/stv2325 , archivePrefix =. 1510.01337 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2325

  12. [12]

    , keywords =

    The milky way total mass profile as inferred from Gaia DR2. , keywords =. doi:10.1093/mnras/staa1017 , archivePrefix =. 1911.04557 , primaryClass =

    work page doi:10.1093/mnras/staa1017 1911

  13. [13]

    The E-MOSAICS Project: simulating the formation and co-evolution of galaxies and their star cluster populations

    The E-MOSAICS project: simulating the formation and co-evolution of galaxies and their star cluster populations. , keywords =. doi:10.1093/mnras/stx3124 , archivePrefix =. 1712.00019 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx3124

  14. [14]

    10, held in Cambridge, England, August 12-15, 1970.)

    Monte Carlo Models of Star Clusters (Part of the Proceedings of the IAU Colloquium No. 10, held in Cambridge, England, August 12-15, 1970.). , year = 1971, month = oct, volume =. doi:10.1007/BF00649159 , adsurl =

    work page doi:10.1007/bf00649159 1970

  15. [15]

    10 Gravitational N-Body Problem (ed

    The Monte Carlo Method (Papers appear in the Proceedings of IAU Colloquium No. 10 Gravitational N-Body Problem (ed. by Myron Lecar), R. Reidel Publ. Co. , Dordrecht-Holland.). , year = 1971, month = nov, volume =. doi:10.1007/BF00649201 , adsurl =

    work page doi:10.1007/bf00649201 1971

  16. [16]

    MOCCA code for star cluster simulations - I. Blue Stragglers, first results

    MOCCA code for star cluster simulations - I. Blue stragglers, first results. , keywords =. doi:10.1093/mnras/sts415 , archivePrefix =. 1207.6700 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sts415

  17. [17]

    A Comprehensive Study of Binary Compact Objects as Gravitational Wave Sources: Evolutionary Channels, Rates, and Physical Properties

    A Comprehensive Study of Binary Compact Objects as Gravitational Wave Sources: Evolutionary Channels, Rates, and Physical Properties. , keywords =. doi:10.1086/340304 , archivePrefix =. astro-ph/0111452 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/340304

  18. [18]

    , keywords =

    Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity. , keywords =. doi:10.1046/j.1365-8711.2000.03426.x , archivePrefix =. astro-ph/0001295 , primaryClass =

    work page doi:10.1046/j.1365-8711.2000.03426.x 2000

  19. [19]

    2002 , month =

    Evolution of binary stars and the effect of tides on binary populations. , keywords =. doi:10.1046/j.1365-8711.2002.05038.x , archivePrefix =. astro-ph/0201220 , primaryClass =

    work page doi:10.1046/j.1365-8711.2002.05038.x 2002

  20. [20]

    , keywords =

    The time-scale of escape from star clusters. , keywords =. doi:10.1046/j.1365-8711.2000.03811.x , archivePrefix =. astro-ph/9910468 , primaryClass =

    work page doi:10.1046/j.1365-8711.2000.03811.x 2000

  21. [21]

    , keywords =

    Absolute V-band magnitudes and mass-to-light ratios of Galactic globular clusters. , keywords =. doi:10.1017/pasa.2020.38 , archivePrefix =. 2009.09611 , primaryClass =

    work page doi:10.1017/pasa.2020.38 2020

  22. [22]

    , keywords =

    Star formation at the smallest scales: a JWST study of the clump populations in SMACS0723. , keywords =. doi:10.1093/mnras/stac3791 , archivePrefix =. 2208.10450 , primaryClass =

    work page doi:10.1093/mnras/stac3791

  23. [23]

    arXiv e-prints , keywords =

    A first GLIMPSE into star clusters populations across cosmic time. arXiv e-prints , keywords =. doi:10.48550/arXiv.2601.16281 , archivePrefix =. 2601.16281 , primaryClass =

    work page doi:10.48550/arxiv.2601.16281

  24. [24]

    2006 , month =

    A statistical study of 233 pulsar proper motions. , keywords =. doi:10.1111/j.1365-2966.2005.09087.x , archivePrefix =. astro-ph/0504584 , primaryClass =

    work page doi:10.1111/j.1365-2966.2005.09087.x 2005

  25. [25]

    2004 , month =

    Stellar collisions during binary-binary and binary-single star interactions. , keywords =. doi:10.1111/j.1365-2966.2004.07914.x , archivePrefix =. astro-ph/0401004 , primaryClass =

    work page doi:10.1111/j.1365-2966.2004.07914.x 2004

  26. [26]

    arXiv e-prints , keywords =

    Spatially Resolved Physical Properties of Young Star Clusters and Star-forming Clumps in the Brightest z>6 Galaxy, the Strongly Lensed Cosmic Spear at z=6.2. arXiv e-prints , keywords =. doi:10.48550/arXiv.2512.08054 , archivePrefix =. 2512.08054 , primaryClass =

    work page doi:10.48550/arxiv.2512.08054

  27. [27]

    , keywords =

    The Sparkler: Evolved High-redshift Globular Cluster Candidates Captured by JWST. , keywords =. doi:10.3847/2041-8213/ac90ca , archivePrefix =. 2208.02233 , primaryClass =

    work page doi:10.3847/2041-8213/ac90ca 2041

  28. [28]

    , keywords =

    Formation of a low-mass galaxy from star clusters in a 600-million-year-old Universe. , keywords =. doi:10.1038/s41586-024-08293-0 , archivePrefix =. 2402.08696 , primaryClass =

    work page doi:10.1038/s41586-024-08293-0

  29. [29]

    Early Results from GLASS-JWST. VII. Evidence for Lensed, Gravitationally Bound Protoglobular Clusters at z = 4 in the Hubble Frontier Field A2744. , keywords =. doi:10.3847/2041-8213/ac8c2d , archivePrefix =. 2208.00520 , primaryClass =

    work page doi:10.3847/2041-8213/ac8c2d 2041

  30. [30]

    , keywords =

    JWST/NIRCam Probes Young Star Clusters in the Reionization Era Sunrise Arc. , keywords =. doi:10.3847/1538-4357/acb59a , archivePrefix =. 2211.09839 , primaryClass =

    work page doi:10.3847/1538-4357/acb59a

  31. [31]

    , keywords =

    JWST spectroscopic confirmation of the Cosmic Gems arc at z = 9.625: Insights into the small-scale structure of a post-burst system. , keywords =. doi:10.1051/0004-6361/202556574 , archivePrefix =. 2507.18705 , primaryClass =

    work page doi:10.1051/0004-6361/202556574

  32. [32]

    , keywords =

    Bound star clusters observed in a lensed galaxy 460 Myr after the Big Bang. , keywords =. doi:10.1038/s41586-024-07703-7 , archivePrefix =. 2401.03224 , primaryClass =

    work page doi:10.1038/s41586-024-07703-7

  33. [33]

    The structure of star clusters. III. Some simple dynamical models. , year = 1966, month = feb, volume =. doi:10.1086/109857 , adsurl =

    work page doi:10.1086/109857 1966

  34. [34]

    2001 , month =

    On the variation of the initial mass function. , keywords =. doi:10.1046/j.1365-8711.2001.04022.x , archivePrefix =. astro-ph/0009005 , primaryClass =

    work page doi:10.1046/j.1365-8711.2001.04022.x 2001

  35. [35]

    The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. I. Overview of the Project and Detection of Multiple Stellar Populations. , keywords =. doi:10.1088/0004-6256/149/3/91 , archivePrefix =. 1410.4564 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/149/3/91

  36. [36]

    The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. IX. The Atlas of Multiple Stellar Populations

    The Hubble Space Telescope UV Legacy Survey of Galactic globular clusters - IX. The Atlas of multiple stellar populations. , keywords =. doi:10.1093/mnras/stw2531 , archivePrefix =. 1610.00451 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw2531

  37. [37]

    Multiple Stellar Populations in Globular Clusters

    Multiple Stellar Populations in Globular Clusters. , keywords =. doi:10.1146/annurev-astro-081817-051839 , archivePrefix =. 1712.01286 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081817-051839

  38. [38]

    , keywords =

    What is a globular cluster? An observational perspective. , keywords =. doi:10.1007/s00159-019-0119-3 , archivePrefix =. 1911.02835 , primaryClass =

    work page doi:10.1007/s00159-019-0119-3 1911

  39. [39]

    , keywords =

    A Family Picture: Tracing the Dynamical Path of the Structural Properties of Multiple Populations in Globular Clusters. , keywords =. doi:10.3847/2041-8213/ab45f7 , archivePrefix =. 1910.00613 , primaryClass =

    work page doi:10.3847/2041-8213/ab45f7 2041

  40. [40]

    , keywords =

    A 3D view of multiple populations' kinematics in Galactic globular clusters. , keywords =. doi:10.1051/0004-6361/202451054 , archivePrefix =. 2409.03827 , primaryClass =

    work page doi:10.1051/0004-6361/202451054

  41. [41]

    , keywords =

    Formation of second-generation stars in globular clusters. , keywords =. doi:10.1093/mnras/stz2055 , archivePrefix =. 1906.09137 , primaryClass =

    work page doi:10.1093/mnras/stz2055 1906

  42. [42]

    2008 , month =

    Formation and dynamical evolution of multiple stellar generations in globular clusters. , keywords =. doi:10.1111/j.1365-2966.2008.13915.x , archivePrefix =. 0809.1438 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.13915.x 2008

  43. [43]

    Rotation and multiple stellar population in globular clusters

    Rotation and Multiple Stellar Population in Globular Clusters. , keywords =. doi:10.1088/2041-8205/724/1/L99 , archivePrefix =. 1010.3841 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/724/1/l99 2041

  44. [44]

    , keywords =

    The role of rotation on the formation of second generation stars in globular clusters. , keywords =. doi:10.1093/mnras/stac2328 , archivePrefix =. 2209.05178 , primaryClass =

    work page doi:10.1093/mnras/stac2328

  45. [45]

    Binary Black Hole Mergers from Globular Clusters: Implications for Advanced LIGO

    Binary Black Hole Mergers from Globular Clusters: Implications for Advanced LIGO. , keywords =. doi:10.1103/PhysRevLett.115.051101 , archivePrefix =. 1505.00792 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.115.051101

  46. [46]

    Binary Black Hole Mergers from Globular Clusters: the Impact of Globular Cluster Properties

    Binary black hole mergers from globular clusters: the impact of globular cluster properties. , keywords =. doi:10.1093/mnras/sty2211 , archivePrefix =. 1808.04514 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2211

  47. [47]

    L., & Bromm, V

    The effect of stellar-mass black holes on the structural evolution of massive star clusters. , keywords =. doi:10.1111/j.1745-3933.2007.00330.x , archivePrefix =. 0704.2494 , primaryClass =

    work page doi:10.1111/j.1745-3933.2007.00330.x 2007

  48. [48]

    2008 , month =

    Black holes and core expansion in massive star clusters. , keywords =. doi:10.1111/j.1365-2966.2008.13052.x , archivePrefix =. 0802.0513 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.13052.x 2008

  49. [49]

    Dynamical evolution of black hole sub-systems in idealised star clusters

    Dynamical evolution of black hole subsystems in idealized star clusters. , keywords =. doi:10.1093/mnras/stt628 , archivePrefix =. 1304.3401 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt628

  50. [50]

    , keywords =

    Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog. , keywords =. doi:10.3847/1538-4365/ab7919 , archivePrefix =. 1911.00018 , primaryClass =

    work page doi:10.3847/1538-4365/ab7919 1911

  51. [51]

    How initial size governs core collapse in globular clusters

    How Initial Size Governs Core Collapse in Globular Clusters. , keywords =. doi:10.3847/1538-4357/aaf646 , archivePrefix =. 1808.02204 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aaf646

  52. [52]

    Natal Kicks of Stellar-Mass Black Holes by Asymmetric Mass Ejection in Fallback Supernovae

    Natal kicks of stellar mass black holes by asymmetric mass ejection in fallback supernovae. , keywords =. doi:10.1093/mnras/stt1106 , archivePrefix =. 1306.0007 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt1106

  53. [53]

    , keywords =

    The dynamical evolution of the stellar clumps in the Sparkler galaxy. , keywords =. doi:10.1051/0004-6361/202554669 , archivePrefix =. 2507.13904 , primaryClass =

    work page doi:10.1051/0004-6361/202554669

  54. [54]

    , keywords =

    Discovery of Ancient Globular Cluster Candidates in the Relic, a Quiescent Galaxy at z = 2.5. , keywords =. doi:10.3847/1538-4357/ae5177 , archivePrefix =. 2501.07627 , primaryClass =

    work page doi:10.3847/1538-4357/ae5177

  55. [55]

    , keywords =

    The Physics of Star Cluster Formation and Evolution. , keywords =. doi:10.1007/s11214-020-00689-4 , archivePrefix =. 2005.00801 , primaryClass =

    work page doi:10.1007/s11214-020-00689-4 2005

  56. [56]

    , keywords =

    Star Clusters Near and Far; Tracing Star Formation Across Cosmic Time. , keywords =. doi:10.1007/s11214-020-00690-x , archivePrefix =. 2005.06188 , primaryClass =

    work page doi:10.1007/s11214-020-00690-x 2005

  57. [57]

    Cosmic wallflowers: the circumgalactic origins of isolated ultra-compact star clusters at $z>7$

    Cosmic wallflowers: the circumgalactic origins of isolated ultra-compact star clusters at z>7. arXiv e-prints , keywords =. doi:10.48550/arXiv.2601.05333 , archivePrefix =. 2601.05333 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2601.05333

  58. [58]

    Compact star clusters in cosmological simulations with a high star formation efficiency and subparsec resolution

    SIEGE: IV. Compact star clusters in cosmological simulations with a high star formation efficiency and subparsec resolution. , keywords =. doi:10.1051/0004-6361/202453252 , archivePrefix =. 2505.06346 , primaryClass =

    work page doi:10.1051/0004-6361/202453252

  59. [59]

    Formation of globular clusters in atomic-cooling halos via rapid gas condensation and fragmentation during the epoch of reionization

    Formation of Globular Clusters in Atomic-cooling Halos Via Rapid Gas Condensation and Fragmentation during the Epoch of Reionization. , keywords =. doi:10.3847/0004-637X/823/1/52 , archivePrefix =. 1510.05671 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/823/1/52

  60. [60]

    , keywords =

    Self-consistent proto-globular cluster formation in cosmological simulations of high-redshift galaxies. , keywords =. doi:10.1093/mnras/staa527 , archivePrefix =. 1906.11261 , primaryClass =

    work page doi:10.1093/mnras/staa527 1906

  61. [61]

    , keywords =

    Formation of proto-globular cluster candidates in cosmological simulations of dwarf galaxies at z > 4. , keywords =. doi:10.1093/mnras/stad1071 , archivePrefix =. 2204.00638 , primaryClass =

    work page doi:10.1093/mnras/stad1071

  62. [62]

    , keywords =

    Star cluster formation and survival in the first galaxies. , keywords =. doi:10.1093/mnras/stad1092 , archivePrefix =. 2212.13946 , primaryClass =

    work page doi:10.1093/mnras/stad1092

  63. [63]

    , keywords =

    Sub-parsec resolution cosmological simulations of star-forming clumps at high redshift with feedback of individual stars. , keywords =. doi:10.1093/mnras/stac2387 , archivePrefix =. 2206.13538 , primaryClass =

    work page doi:10.1093/mnras/stac2387

  64. [64]

    The formation of dense stellar clusters in sub-parsec resolution cosmological simulations with individual star feedback

    SIEGE: III. The formation of dense stellar clusters in sub-parsec resolution cosmological simulations with individual star feedback. , keywords =. doi:10.1051/0004-6361/202452876 , archivePrefix =. 2411.02502 , primaryClass =

    work page doi:10.1051/0004-6361/202452876

  65. [65]

    Globular clusters as the relics of regular star formation in 'normal' high-redshift galaxies

    Globular clusters as the relics of regular star formation in `normal' high-redshift galaxies. , keywords =. doi:10.1093/mnras/stv2026 , archivePrefix =. 1509.02163 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2026

  66. [66]

    Mass Evaporation Rate of Globular Clusters in a Strong Tidal Field

    Mass evaporation rate of globular clusters in a strong tidal field. , keywords =. doi:10.1093/mnras/stx1350 , archivePrefix =. 1706.06635 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1350

  67. [67]

    2001 , month =

    Scaling of N-body calculations. , keywords =. doi:10.1046/j.1365-8711.2001.04272.x , archivePrefix =. astro-ph/0012330 , primaryClass =

    work page doi:10.1046/j.1365-8711.2001.04272.x 2001

  68. [68]

    Treatment of realistic tidal field in Monte Carlo simulations of star clusters

    Treatment of realistic tidal field in Monte Carlo simulations of star clusters. , keywords =. doi:10.1093/mnras/stu1426 , archivePrefix =. 1407.4169 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu1426

  69. [69]

    , keywords =

    Escape from a tidally limited star cluster. , keywords =. doi:10.1093/mnras/284.4.811 , adsurl =

    work page doi:10.1093/mnras/284.4.811

  70. [70]

    Dynamical Evolution of Globular Clusters in Hierarchical Cosmology

    Dynamical Evolution of Globular Clusters in Hierarchical Cosmology. , keywords =. doi:10.1086/591777 , archivePrefix =. astro-ph/0608069 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/591777

  71. [71]

    Effects of Tidal Shocks on the Evolution of Globular Clusters

    Effects of Tidal Shocks on the Evolution of Globular Clusters. , keywords =. doi:10.1086/307659 , archivePrefix =. astro-ph/9806245 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/307659

  72. [72]

    , keywords =

    Tidal-Shock Relaxation: A Reexamination of Tidal Shocks in Stellar Systems. , keywords =. doi:10.1086/175114 , adsurl =

    work page doi:10.1086/175114

  73. [73]

    Destruction of the Galactic Globular Cluster System

    Destruction of the Galactic Globular Cluster System. , keywords =. doi:10.1086/303441 , archivePrefix =. astro-ph/9603042 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/303441

  74. [74]

    The Effect of the Galactic Spheroid on Globular Cluster Evolution

    The effect of the Galactic spheroid on globular cluster evolution. , keywords =. doi:10.1093/mnras/288.3.749 , archivePrefix =. astro-ph/9604049 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/288.3.749

  75. [75]

    , year = 1972, month = sep, volume =

    On the Evolution of Globular Clusters. , year = 1972, month = sep, volume =. doi:10.1086/181018 , adsurl =

    work page doi:10.1086/181018 1972

  76. [76]

    , keywords =

    Dynamical evolution of multiple-population globular clusters. , keywords =. doi:10.1093/mnras/stab223 , archivePrefix =. 2102.01717 , primaryClass =

    work page doi:10.1093/mnras/stab223

  77. [77]

    Dissolution of tidally filling star clusters harbouring black hole subsystems

    MOCCA survey data base- I. Dissolution of tidally filling star clusters harbouring black hole subsystems. , keywords =. doi:10.1093/mnras/stz1460 , archivePrefix =. 1904.01227 , primaryClass =

    work page doi:10.1093/mnras/stz1460 1904

  78. [78]

    MOCCA Code for Star Cluster Simulations - II. Comparison with N-body Simulations

    MOCCA code for star cluster simulations - II. Comparison with N-body simulations. , keywords =. doi:10.1093/mnras/stt307 , archivePrefix =. 1112.6246 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt307

  79. [79]

    Million-Body Star Cluster Simulations: Comparisons between Monte Carlo and Direct $N$-body

    Million-body star cluster simulations: comparisons between Monte Carlo and direct N-body. , keywords =. doi:10.1093/mnras/stw2121 , archivePrefix =. 1601.04227 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw2121

  80. [80]

    , keywords =

    The structural properties of multiple populations in the dynamically young globular cluster NGC 2419. , keywords =. doi:10.1051/0004-6361/202346792 , archivePrefix =. 2307.09508 , primaryClass =

    work page doi:10.1051/0004-6361/202346792

Showing first 80 references.