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REVIEW 3 major objections 4 minor 288 references

Does IRS13 require an intermediate-mass black hole?

T0 review · 3 major / 4 minor · reviewed 2026-08-14 · deepseek-v4-flash

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Pith's one-line read IRS13 is a transient stellar overdensity, not a bound cluster requiring an intermediate-mass black hole.

desk verdict A clear proceedings recap of Pavlík et al. 2024, arguing IRS13 is a transient tidal overdensity rather than an IMBH host; the headline conclusion isn't new here, and the modeling equivalence is under-specified. read the letter →

arxiv 2608.10117 v1 pith:ETMQNMAM submitted 2026-08-10 astro-ph.GA

Václav Pavlík , Vladimír Karas , Florian Pei{ss}ker , Bhavana Bhat , Andreas Eckart This is my paper · ORCID
classification astro-ph.GA
keywords GalacticcenterIRS13intermediate-massblackholeN-bodysimulationstidaldisruptionphase-spaceoverdensitystellarkinematicsstarclusters
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper asks whether the compact stellar association IRS13 near Sagittarius A* requires an intermediate-mass black hole (IMBH) to remain bound. Using direct N-body simulations, it shows that an IRS13-sized cluster of 44 stars dissolves within a fraction of a million years even when an IMBH of $4\times10^4$ solar masses is present. The observed velocity dispersion can arise naturally from the tidal field of Sgr A* and from the infall event, so it does not imply a central IMBH. The authors conclude that IRS13 is best viewed as a temporary phase-space overdensity, analogous to phase-wrapped shells and streams in disrupted galaxies. This matters because it removes a key piece of evidence for an IMBH at the Galactic center and reframes IRS13 as a continuously changing debris structure.

What carries the argument

The central mechanism is the combination of the Sgr A* tidal field and internal dynamical heating from a hard star-IMBH binary. The paper uses direct N-body simulations of two setups: small 44-star clusters on circular and eccentric orbits, with and without an IMBH, and more massive clusters falling from 10-100 pc. Tidal stripping at pericentre removes stars, while the hard binary scatters stars and ejects them, together dissolving the cluster within a fraction of a Myr. The result is a phase-space overdensity: a set of stars that appear clustered in position and velocity but are not gravitationally bound, and which disperses through phase mixing.

What would settle it

Precise proper-motion measurements of IRS13 members over several years would settle the question: if they show a stable, bound, rotating core persisting over a full orbit, then the transient-overdensity picture is wrong, whereas a gradually dispersing clump without coherent internal rotation would support it.

Watch

Extended reading notes

Core claim

The central claim is that IRS13 does not require an intermediate-mass black hole to hold itself together. The paper's N-body models show that an initially virialised cluster of 44 equal-mass stars, with or without an embedded IMBH up to $4\times10^4$ solar masses, dissolves within a fraction of a million years in the tidal field of Sgr A*. The most massive IMBH considered actually accelerates disruption by forming a hard star-IMBH binary that ejects stars. In simulations of larger infalling clusters, tidal stripping produces transient disks, spiral-like streams, and ring-like overdensities that phase-mix away. The authors interpret IRS13 as one such temporary overdensity, implying that its measured velocity dispersion cannot be used to infer an IMBH's presence or mass.

Load-bearing premise

The simulations assume that IRS13 can be modeled as a single infalling cluster of 44 equal-mass stars, initially virialised, with or without a central IMBH, and that the Galactic potential is dominated by Sgr A* plus an external field; if the real IRS13 is more massive, more compact, or formed from multiple unrelated populations, the dissolution timescale and the 'no-IMBH' conclusion would not directly apply.

Editorial extensions

If this is right

  • The velocity dispersion of IRS13 members cannot by itself constrain the presence or mass of an IMBH at the Galactic center.
  • IRS13 should be treated as a continuously evolving stellar grouping, not a relaxed bound cluster, so its stellar population and dynamics change on short timescales.
  • Tidal disruption of infalling clusters can naturally populate the central parsec with IRS13-like overdensities, so similar associations elsewhere need not be gravitationally bound.
  • Eccentric orbits slow the disruption but do not prevent it, while more massive IMBHs accelerate it through dynamical heating.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If IRS13 is a transient tidal-debris structure, then similar compact stellar associations in other galactic nuclei may also be debris, and their velocity dispersions should not be converted into enclosed masses without tidal and infall modelling.
  • A decisive observational test is precise proper motions of IRS13 members: if they show a persistent, bound, rotating core over a full orbit, the transient-overdensity picture would be falsified.
  • The shell analogy suggests that the infalling-cluster scenario predicts faint, large-scale streams or ripples in the inner Galaxy along the orbital path, which deep imaging could search for.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. This proceedings paper investigates whether the Galactic-centre association IRS13 requires an intermediate-mass black hole (IMBH) to remain bound. The authors use two suites of direct N-body simulations: (i) IRS13-like clusters consisting of 44 equal-mass stars (1 or 10 M_sun), initially virialised, on circular and eccentric orbits around Sgr A*, with or without embedded IMBHs of mass 10^3 and 4x10^4 M_sun; and (ii) more massive infalling clusters (N ~ 20,000-50,000) evolved with the PETAR code in an external potential that includes Sgr A* and a putative IMBH. They report that the orbiting clusters dissolve within a fraction of a Myr even with the most massive IMBH considered, that the observed velocity dispersion can arise from the tidal field and infall rather than an IMBH, and that IRS13 is best interpreted as a transient phase-space overdensity analogous to shells and streams in disrupted galaxies. Quantitative details and full parameter-space analysis are deferred to Pavlik et al. (2024).

Significance. If the central claim holds, it would weaken the dynamical evidence for an IMBH in IRS13 and place the association in a broader tidal-disruption and phase-mixing context. The paper's strengths are its use of established direct N-body codes (REBOUND, PETAR), clearly stated broad initial-condition choices, and an explicit observational test (searching for phase-space substructure). The morphological analogy in Fig. 3 is suggestive. However, the presented evidence is largely qualitative and relies heavily on the companion paper; the load-bearing modeling assumptions are not fully specified or validated against observations, so the significance is conditional.

major comments (3)
  1. [§2.1, Figs. 1-2] The initial conditions for the orbiting-cluster runs are not fully specified: the clusters are described as containing 44 equal-mass stars (1 or 10 M_sun) and being initially virialised, but the initial cluster radius, half-mass radius, concentration, and orbital phase are not given. The dissolution timescale and the conclusion that an IMBH cannot keep IRS13 bound depend sensitively on cluster density and size, since a more compact or more massive cluster has a longer relaxation time and a larger tidal radius. Without showing that these models lie within the observed parameter range of IRS13, the 'no IMBH required' conclusion is not established for the actual association.
  2. [Abstract; §3] The abstract asserts that the observed velocity dispersion 'can arise naturally from the tidal field of Sgr A* and the infall event itself,' but this paper does not provide any quantitative comparison between the simulated velocity dispersions and the observed IRS13 kinematics. The reader cannot verify that the proposed mechanism reproduces the magnitude and character of the observed dispersion, or that the simulated phase-space distribution matches the data. This claim should either be demonstrated here with a figure or table, or explicitly identified as a result of Pavlik et al. (2024) with a pointer to the specific analysis.
  3. [§2.2, Fig. 3] The infalling-cluster simulations are said to explore a range of cluster masses, sizes, and orbital parameters, but the illustrative runs in Fig. 3 all appear to start at 10 pc from Sgr A* and differ only in particle number (20k vs 50k) and tangential velocity; no radial scan is shown. More importantly, the paper does not quantify how many stars are deposited into the central parsec, the resulting surface-density profile, or the velocity dispersion of the deposited material. Without such quantitative output, the claim that infalling clusters 'naturally produce IRS13-like stellar overdensities' remains a qualitative suggestion rather than a demonstrated result.
minor comments (4)
  1. [§2.1] The numerical integration scheme used for the REBOUND runs (e.g., IAS15 vs. WHFast) is not stated; specifying it would improve reproducibility.
  2. [Figs. 1-2 captions] The captions refer to 'the black trajectory' of the cluster, but in the figures the trajectory is not clearly distinguishable from the plotted stellar points; a distinct line style or annotation would help the reader follow the orbit.
  3. [Abstract; §3] The term 'phase-space overdensity' is used repeatedly but is never defined; a one-sentence definition (for example, a grouping in position-velocity space that is not necessarily gravitationally bound) would make the paper more accessible to the proceedings readership.
  4. [Footnote, §2.1] The footnote cites Reid and Brunthaler (2004) to exclude a 4e4 M_sun IMBH close to Sgr A*, but that reference primarily constrains the mass and proper motion of Sgr A* itself; the authors should verify that this citation directly supports the stated exclusion or replace it with a more specific dynamical constraint.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the dissolution and velocity-dispersion claims are direct N-body outputs, not refits or self-citation-defined results.

full rationale

The paper's central claims—that a 44-star IRS13-sized cluster dissolves within a fraction of a Myr even with a 4e4 Msun IMBH, and that the observed velocity dispersion can be a product of the Sgr A* tidal field and infall—are outputs of direct N-body integrations (REBOUND and PETAR) with stated initial conditions. No parameter is fitted to the observed IRS13 velocity dispersion in the text; the dispersion conclusion is a dynamical consequence of the modeled tidal disruption, not a re-labeled input. The self-citations to Pavlik et al. 2024 summarize the same simulation campaign and represent reproducible N-body evidence, so they do not function as an unverified definitional premise; the paper also presents illustrative cases in Figs. 1-3. The hand-chosen initial conditions (44 equal-mass stars of 1 or 10 solar masses, virialised, varied IMBH mass and orbit) are an assumption-sensitivity concern but do not make the conclusion true by construction. The footnote on p. 2 itself notes that a 4e4 Msun IMBH so close to Sgr A* has been excluded by external work, which limits the physical relevance of that branch but is not circularity. The quantitative velocity-dispersion comparison is delegated to Pavlik et al. 2024 rather than fully reproduced here, but this is a missing-detail issue, not a circular reduction.

Assumptions & free parameters 5 free parameters · 4 assumptions · 0 invented entities

The paper introduces no new physical entities. The free parameters are simulation initial conditions and the assumed IMBH mass, all chosen by hand. The axioms are standard dynamical modeling assumptions, with the IRS13-as-44-equal-mass-cluster premise being an ad hoc simplification that directly affects the central dissolution result.

free parameters (5)
  • Embedded IMBH mass in orbiting-cluster runs = 10^3 and 4x10^4 solar masses
    Chosen by hand to bracket the IRS13 IMBH hypothesis from Peissker et al. 2023; the upper value is noted in a footnote to be excluded by astrometry of Sgr A*.
  • Initial stellar mass in orbiting-cluster runs = 1 or 10 solar masses (equal-mass)
    Simplified equal-mass stellar populations; the paper states this choice without justification.
  • Infalling cluster particle number = 20,000 and 50,000
    Chosen for the second suite; representative values shown in Fig. 3, full range delegated to Pavlik et al. 2024.
  • Infalling cluster initial distance and tangential velocity = 10 pc; 5, 10, 20 km/s
    Illustrative initial conditions for the infalling-cluster models in Fig. 3.
  • IMBH orbital radius in infalling runs = 0.4 pc
    Fixed circular orbit for the putative IMBH during infall simulations; not varied in the text.
assumptions (4)
  • domain assumption Newtonian N-body dynamics accurately describe the cluster evolution near Sgr A*; relativistic effects and stellar collisions are neglected.
    The method section invokes direct N-body integration with REBOUND and PETAR without discussing post-Newtonian corrections or collisional processes.
  • ad hoc to paper IRS13 can be modeled as an initially virialised cluster of 44 equal-mass stars.
    Sec. 2.1 assumes this initial configuration based on the observed source count and simplified masses; the observed cluster may not be virialised or single-population.
  • domain assumption The Galactic potential is dominated by Sgr A* (and a possible IMBH), with the infalling-cluster runs adding an unspecified external Galactic potential.
    Sec. 2.2 states clusters evolved in the external Galactic potential without specifying the potential model or other perturbers such as giant molecular clouds or the stellar cusp.
  • domain assumption A hard star-IMBH binary forms naturally in the runs and drives dynamical heating.
    Sec. 2.1 states this as a finding; it assumes three-body interactions are resolved by the N-body code.

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Cite this review

Pith. "Pith review of Does IRS13 require an intermediate-mass black hole?." pith.science (2026). https://pith.science/paper/ETMQNMAM

@misc{pith2026260810117,
  author       = {Pith},
  title        = {Pith review of: Does IRS13 require an intermediate-mass black hole?},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ETMQNMAM}},
  note         = {Machine review of arXiv:2608.10117}
}
abstract

We investigate whether the Galactic-centre association IRS13 requires an intermediate-mass black hole (IMBH) to remain bound. Using high-precision $N$-body calculations of IRS13-like systems orbiting the Milky Way supermassive black hole (SMBH), as well as simulations of more massive infalling clusters, we find that an IRS13-sized cluster dissolves on a very short timescale even when an IMBH of $4\times10^4\,M_\odot$ is present. The observed velocity dispersion can arise naturally from the tidal field of Sgr A* and the infall event itself; therefore, it need not imply a central IMBH. In the infalling-cluster runs, tidal stripping produces transient disks, spiral-like structures, and ring-like overdensities. These features suggest a broader interpretation: IRS13 is best viewed as a temporary phase-space overdensity, analogous in mechanism (though not in scale) to phase-wrapped shells and streams in disrupted galaxies.

Figures

Figures reproduced from arXiv: 2608.10117 by the authors.

Figure 1
Figure 1. Snapshots illustrating the tidal disruption of representative IRS13-like models on initially circular orbits around Sgr A* (as the black trajectory shows). The stars are initially bound to the IMBH (black circle) but rapidly disperse – red points denote stars bound to the IMBH (with red curves showing their instantaneous osculating Keplerian orbits), whereas grey points represent unbound stars. The stellar mass is 1… view at source ↗
Figure 2
Figure 2. Same as [PITH_FULL_IMAGE:figures/full_fig_p002_2.png] view at source ↗
Figure 3
Figure 3. Illustrative snapshots of five simulated infalling cluster models (the initial number of stars, dis￾tance from Sgr A* in the x direction, and tangential velocity are indicated in the corner of each row). The colour scale shows the number of stars in each bin. The red cross marks the position of Sgr A* (orbited by the IMBH at 0.4 pc, see the red circle). Tidal stripping during successive passages through the Galactic… view at source ↗

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Works this paper leans on

288 extracted references · 30 canonical work pages

  1. [1]

    , keywords =

    Intermediate-mass Black Holes in Early Globular Clusters. , keywords =. doi:10.1088/2041-8205/713/1/L41 , archivePrefix =. 1003.3470 , primaryClass =

    arXiv

  2. [2]

    , keywords =

    Intermediate-mass Black Hole Progenitors from Stellar Collisions in Dense Star Clusters. , keywords =. doi:10.3847/1538-4357/ad43d6 , archivePrefix =. 2404.11646 , primaryClass =

    arXiv

  3. [3]

    , keywords =

    Formation of massive black holes through runaway collisions in dense young star clusters. , keywords =. doi:10.1038/nature02448 , archivePrefix =. astro-ph/0402622 , primaryClass =

    arXiv

  4. [4]

    , keywords =

    NBODY6++GPU: ready for the gravitational million-body problem. , keywords =. doi:10.1093/mnras/stv817 , archivePrefix =. 1504.03687 , primaryClass =

    arXiv

  5. [5]

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

    doi:10.1086/109857 1966

  6. [6]

    , keywords =

    AGAMA: action-based galaxy modelling architecture. , keywords =. doi:10.1093/mnras/sty2672 , archivePrefix =. 1802.08239 , primaryClass =

    arXiv

  7. [7]

    Aarseth, S. J. , title =

  8. [8]

    Dynamical evolution of globular clusters

Show all 288 references
  1. [10]

    Aarseth, S. J. , editor =. Binary Evolution in Stellar Systems , bookTitle =. 1972 , publisher =

    1972

  2. [11]

    Plummer, H. C. , title =. , year = 1911, month = mar, volume =

    1911

  3. [12]

    Salpeter, E. E. , title =. , year = 1955, month = jan, volume = 121, pages =. doi:10.1086/145971 , adsurl =

    1955 doi

  4. [13]

    Heggie, D. C. and Hut, P. , title =

  5. [14]

    , keywords =

    Binaries as a heat source in stellar dynamics - Release of binding energy. , keywords =. doi:10.1086/184111 , adsurl =

    doi

  6. [15]

    and Hut, P

    Casertano, S. and Hut, P. , title =. , keywords =. doi:10.1086/163589 , adsurl =

    doi

  7. [16]

    Journal of Computational Physics , year = 1973, volume = 12, pages =

    A numerical integration scheme for the N-body gravitational problem. Journal of Computational Physics , year = 1973, volume = 12, pages =. doi:10.1016/0021-9991(73)90160-5 , adsurl =

    1973 doi

  8. [17]

    Fujii, M. S. and Portegies Zwart, S. , title =. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stu015 , adsurl =

    doi

  9. [18]

    O'Leary, R. M. and Stahler, S. W. and Ma, C.-P. , title =. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stu1455 , adsurl =

    doi

  10. [19]

    and Aarseth, S

    Spurzem, R. and Aarseth, S. J. , title =. , eprint =. doi:10.1093/mnras/282.1.19 , adsurl =

    doi

  11. [21]

    , eprint =

    Postcollapse Evolution of Globular Clusters. , eprint =. doi:10.1086/178007 , adsurl =

    doi

  12. [22]

    IAU Symposium , volume = 174, pages =

    Gravothermal Oscillations. IAU Symposium , volume = 174, pages =

  13. [25]

    , eprint =

    Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity. , eprint =. doi:10.1046/j.1365-8711.2000.03426.x , adsurl =

  14. [27]

    , keywords =

    On the Maximum Mass of Stellar Black Holes. , keywords =. doi:10.1088/0004-637X/714/2/1217 , archivePrefix =. 0904.2784 , primaryClass =

    arXiv

  15. [28]

    2008 , publisher=

    Galactic Dynamics: 2nd Ed , author=. 2008 , publisher=

    2008

  16. [29]

    , keywords =

    Masses and mass-to-light ratios of galaxies. , keywords =. doi:10.1146/annurev.aa.17.090179.001031 , adsurl =

  17. [30]

    , archivePrefix = "arXiv", eprint =

    The Galaxy in Context: Structural, Kinematic, and Integrated Properties. , archivePrefix = "arXiv", eprint =. doi:10.1146/annurev-astro-081915-023441 , adsurl =

    doi

  18. [31]

    Constraining the initial conditions of young stellar clusters by studying their binary populations

    Inverse dynamical population synthesis. Constraining the initial conditions of young stellar clusters by studying their binary populations. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201118231 , adsurl =

    doi

  19. [32]

    , keywords =

    Dynamical population synthesis: constructing the stellar single and binary contents of galactic field populations. , keywords =. 2011. doi:10.1111/j.1365-2966.2011.19519.x , archivePrefix =. 1109.2896 , primaryClass =

    2011

  20. [33]

    Random Gravitational Encounters and the Evolution of Spherical Systems. I. Method. , year = 1971, month = mar, volume = 164, pages =. doi:10.1086/150855 , adsurl =

    1971 doi

  21. [34]

    Random Gravitational Encounters and the Evolution of Spherical Systems. II. Models. , year = 1971, month = jun, volume = 166, pages =. doi:10.1086/150977 , adsurl =

    1971 doi

  22. [35]

    Mass segregation and fractal substructure in young massive clusters – I

    K. Mass segregation and fractal substructure in young massive clusters – I. The McLuster code and method calibration , journal =. 2011 , doi =

    2011

  23. [36]

    , keywords =

    Neutron stars and millisecond pulsars in star clusters: implications for the diffuse gamma-radiation from the Galactic Centre. , keywords =. 2018. doi:10.1093/mnras/sty2234 , archivePrefix =. 1804.04856 , primaryClass =

    2018 arXiv

  24. [37]

    A MODEST review

    Varri, Anna Lisa and Cai, Maxwell Xu and Concha-Ram \'i rez, Francisca and Dinnbier, Franti s ek and L \"u tzgendorf, Nora and Pavl \'i k, V \'a clav and Rastello, Sara and Sollima, Antonio and Wang, Long and Zocchi, Alice. A MODEST review. Computational Astrophysics and Cosmo...

    2018 doi

  25. [38]

    , keywords =

    The hunt for self-similar core collapse. , keywords =. doi:10.1051/0004-6361/201833854 , archivePrefix =. 1808.05230 , primaryClass =

    arXiv

  26. [39]

    , keywords =

    The black hole retention fraction in star clusters. , keywords =. doi:10.1051/0004-6361/201832919 , primaryClass =

    doi

  27. [40]

    , keywords =

    Do star clusters form in a completely mass-segregated way?. , keywords =. 2019. doi:10.1051/0004-6361/201834265 , archivePrefix =. 1905.09289 , primaryClass =

    2019 arXiv

  28. [41]

    CAOSP , keywords =

    Primordial mass segregation of star clusters: The role of binary stars. CAOSP , keywords =. doi:10.31577/caosp.2020.50.2.456 , archivePrefix =. 2001.01450 , primaryClass =

    2020 arXiv

  29. [42]

    , keywords =

    Primordial mass segregation of star clusters with primordial binaries. , keywords =. doi:10.1051/0004-6361/202037490 , archivePrefix =. 2004.14389 , primaryClass =

    2004 arXiv

  30. [43]

    VizieR Online Data Catalog , keywords =

    VizieR Online Data Catalog: ONC stars masses from literature (Pavlik+, 2019). VizieR Online Data Catalog , keywords =. 2019

    2019

  31. [44]

    Planets, Stars and Stellar Systems

    The Stellar and Sub-Stellar Initial Mass Function of Simple and Composite Populations. Planets, Stars and Stellar Systems. Volume 5: Galactic Structure and Stellar Populations , year = 2013, editor =. doi:10.1007/978-94-007-5612-0_4 , adsurl =

    2013 doi

  32. [45]

    Estimating Distance from Parallaxes. IV. Distances to 1.33 Billion Stars in Gaia Data Release 2. , keywords =. doi:10.3847/1538-3881/aacb21 , primaryClass =

    doi

  33. [46]

    ArXiv e-prints , archivePrefix = "arXiv", eprint =

    3D shape of Orion A from Gaia DR2. ArXiv e-prints , archivePrefix = "arXiv", eprint =

  34. [47]

    VizieR Online Data Catalog , keywords =

    VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003). VizieR Online Data Catalog , keywords =

    2003

  35. [48]

    , keywords =

    The Fourth US Naval Observatory CCD Astrograph Catalog (UCAC4). , keywords =. doi:10.1088/0004-6256/145/2/44 , archivePrefix =. 1212.6182 , primaryClass =

    arXiv

  36. [49]

    Protostars and Planets VI , archivePrefix = "arXiv", eprint =

    From Filamentary Networks to Dense Cores in Molecular Clouds: Toward a New Paradigm for Star Formation. Protostars and Planets VI , archivePrefix = "arXiv", eprint =. doi:10.2458/azu_uapress_9780816531240-ch002 , adsurl =

    doi

  37. [50]

    , keywords =

    Fibers in the NGC 1333 proto-cluster. , keywords =. doi:10.1051/0004-6361/201630348 , archivePrefix =. 1703.07029 , primaryClass =

    arXiv

  38. [51]

    An ALMA study of the Orion Integral Filament. I. Evidence for narrow fibers in a massive cloud. , keywords =. doi:10.1051/0004-6361/201731894 , archivePrefix =. 1801.01500 , primaryClass =

    arXiv

  39. [52]

    , keywords =

    A Modified Aarseth Code for GRAPE and Vector Processors. , keywords =

  40. [53]

    , keywords =

    On a Hermite integrator with Ahmad-Cohen scheme for gravitational many-body problems. , keywords =

  41. [54]

    doi:10.1515/crll.1965.218.204 , issn =

    Journal f. doi:10.1515/crll.1965.218.204 , issn =

    1965 doi

  42. [55]

    Celestial Mechanics , keywords =

    A regularization of the three-body problem. Celestial Mechanics , keywords =. doi:10.1007/BF01227619 , adsurl =

    doi

  43. [56]

    Celestial Mechanics and Dynamical Astronomy , keywords =

    An implementation of N-body chain regularization. Celestial Mechanics and Dynamical Astronomy , keywords =. doi:10.1007/BF00695714 , adsurl =

    doi

  44. [57]

    Celestial Mechanics and Dynamical Astronomy , keywords =

    A chain regularization method for the few-body problem. Celestial Mechanics and Dynamical Astronomy , keywords =

  45. [58]

    1950", month =

    The Electrical Conductivity of an Ionized Gas. Physical Review , year = "1950", month = "Oct", volume =. doi:10.1103/PhysRev.80.230 , adsurl =

    1950 doi

  46. [59]

    I - The hybrid code

    A unified N-body and statistical treatment of stellar dynamics. I - The hybrid code. , keywords =. 1984. doi:10.1086/162366 , adsurl =

    1984 doi

  47. [60]

    1971", month =

    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 =

    1970 doi

  48. [61]

    1971", month =

    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 =

    1971 doi

  49. [62]

    1973", month =

    Numerical Experiments on the Stability of Spherical Stellar Systems. , year = "1973", month = "Apr", volume =

    1973

  50. [63]

    1972", month =

    Random Gravitational Encounters and the Evolution of Spherical Systems. IV Isolated Systems of Identical Stars. , year = "1972", month = "Jul", volume =. doi:10.1086/151537 , adsurl =

    1972 doi

  51. [64]

    II - Distribution of the orbital elements in an unbiased sample

    Multiplicity among solar-type stars in the solar neighbourhood. II - Distribution of the orbital elements in an unbiased sample. , keywords =. 1991

    1991

  52. [65]

    The Astrophysical Journal Supplement Series , keywords =

    A Survey of Stellar Families: Multiplicity of Solar-type Stars. The Astrophysical Journal Supplement Series , keywords =. 2010. doi:10.1088/0067-0049/190/1/1 , archivePrefix =. 1007.0414 , primaryClass =

    2010 arXiv

  53. [66]

    , keywords =

    Interrupted Stellar Encounters in Star Clusters. , keywords =. 2015. doi:10.1088/2041-8205/808/1/L25 , archivePrefix =. 1506.08830 , primaryClass =

    2015 arXiv

  54. [67]

    Roaming the realm of not-so-small-N

    Small-N collisional dynamics - II. Roaming the realm of not-so-small-N. , keywords =. 2015. doi:10.1093/mnras/stv685 , archivePrefix =. 1503.07876 , primaryClass =

    2015 arXiv

  55. [68]

    Dynamical Friction. I. General Considerations: the Coefficient of Dynamical Friction. , year = 1943, month = mar, volume =. doi:10.1086/144517 , adsurl =

    1943 doi

  56. [69]

    1942", month =

    The Statistics of the Gravitational Field Arising from a Random Distribution of Stars. I. The Speed of Fluctuations. , year = "1942", month = "May", volume =. doi:10.1086/144420 , adsurl =

    1942 doi

  57. [70]

    1943", month =

    The Statistics of the Gravitational Field Arising from a Random Distribution of Stars II. , year = "1943", month = "Jan", volume =. doi:10.1086/144487 , adsurl =

    1943 doi

  58. [71]

    , keywords =

    A numerical approach to the testing of the fission hypothesis. , keywords =. doi:10.1086/112164 , adsurl =

    doi

  59. [72]

    Monaghan, J. J. and Gingold, R. A. , title = ". , volume =. 1977 , month =. doi:10.1093/mnras/181.3.375 , url =

    1977 doi

  60. [73]

    Heggie, D. C. , title = "

  61. [74]

    Heggie, D. C. and Mathieu, R. D. , editor =. Standardised units and time scales. The Use of Supercomputers in Stellar Dynamics. 1986

    1986

  62. [75]

    , eprint =

    Modeling the Disruption of the Globular Cluster Palomar 5 by Galactic Tides. , eprint =. doi:10.1086/383214 , adsurl =

    doi

  63. [77]

    and Kroupa, P

    Dinnbier, F. and Kroupa, P. , title =. Modelling and Observing Dense Stellar Systems (MODEST-19) , year = 2019, series =

    2019

  64. [78]

    , archivePrefix = "arXiv", eprint =

    Constraining the Milky Way mass with hypervelocity stars. , archivePrefix = "arXiv", eprint =. doi:10.1016/j.newast.2017.03.002 , adsurl =

    2017 doi

  65. [79]

    , archivePrefix = "arXiv", eprint =

    High-velocity stars from the interaction of a globular cluster and a massive black hole binary. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stw531 , adsurl =

    doi

  66. [80]

    , archivePrefix = "arXiv", eprint =

    Stellar Multiplicity. , archivePrefix = "arXiv", eprint =. doi:10.1146/annurev-astro-081710-102602 , adsurl =

    doi

  67. [81]

    , archivePrefix = "arXiv", eprint =

    Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection. , archivePrefix = "arXiv", eprint =. doi:10.1088/0067-0049/215/1/15 , adsurl =

    doi

  68. [82]

    II - Distribution of the orbital elements in an unbiased sample

    Multiplicity among solar-type stars in the solar neighbourhood. II - Distribution of the orbital elements in an unbiased sample. A& A , year = 1991, month = ago, volume = 248, pages =. doi:1991A&A...248..485D , adsurl =

    1991

  69. [83]

    A Survey of Stellar Families: Multiplicity of Solar-type Stars. Suppl. , year = 2010, month = sep, volume = 190, pages =. doi:10.1088/0067-0049/190/1/1 , adsurl =

    2010 doi

  70. [84]

    , year = 2006, month = jul, volume = 646, pages =

    Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems. , year = 2006, month = jul, volume = 646, pages =. doi:10.1086/504823 , adsurl =

    2006 doi

  71. [85]

    New low-mass stellar companions of the exoplanet host stars HD 125612 and HD 212301

    The multiplicity of exoplanet host stars. New low-mass stellar companions of the exoplanet host stars HD 125612 and HD 212301. A& A , year = 2009, month = jan, volume = 494, pages =. doi:10.1051/0004-6361:200810639 , adsurl =

    2009 doi

  72. [86]

    A& A , year = 2012, month = jun, volume = 542, pages =

    Extrasolar planets in stellar multiple systems. A& A , year = 2012, month = jun, volume = 542, pages =. doi:10.1051/0004-6361/201118051 , adsurl =

    2012 doi

  73. [87]

    From Binaries to Multiples. I. Data on F and G Dwarfs within 67 pc of the Sun. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-6256/147/4/86 , adsurl =

    doi

  74. [88]

    From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-6256/147/4/87 , adsurl =

    doi

  75. [89]

    , archivePrefix = "arXiv", eprint =

    A Survey of the High Order Multiplicity of Nearby Solar-type Binary Stars with Robo-AO. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/799/1/4 , adsurl =

    doi

  76. [90]

    , year = 1962, month = nov, volume = 67, pages =

    Secular perturbations of asteroids with high inclination and eccentricity. , year = 1962, month = nov, volume = 67, pages =. doi:10.1086/108790 , adsurl =

    1962 doi

  77. [91]

    , year = 1962, month = oct, volume = 9, pages =

    The evolution of orbits of artificial satellites of planets under the action of gravitational perturbations of external bodies. , year = 1962, month = oct, volume = 9, pages =. doi:10.1016/0032-0633(62)90129-0 , adsurl =

    1962 doi

  78. [92]

    , keywords =

    Tidal interactions in star cluster simulations. , keywords =. doi:10.1046/j.1365-8711.2001.03974.x , adsurl =

    2001

  79. [93]

    , year = 1996, month = oct, volume = 282, pages =

    The Effect of Encounters on the Eccentricity of Binaries in Clusters. , year = 1996, month = oct, volume = 282, pages =. doi:10.1093/mnras/282.3.1064 , adsurl =

    1996 doi

  80. [95]

    Identical point-particles

    The chaotic four-body problem in Newtonian gravity- I. Identical point-particles. , year = 2016, month = dec, volume = 463, pages =. doi:10.1093/mnras/stw2178 , adsurl =

    2016 doi

  81. [96]

    , year = 2016, month = aug, volume = 460, pages =

    New prospects for observing and cataloguing exoplanets in well-detached binaries. , year = 2016, month = aug, volume = 460, pages =. doi:10.1093/mnras/stw1218 , adsurl =

    2016 doi

  82. [97]

    Suppl , year = 2014, month = feb, volume = 210, pages =

    Planetary Candidates Observed by Kepler IV: Planet Sample from Q1-Q8 (22 Months). Suppl , year = 2014, month = feb, volume = 210, pages =. doi:10.1088/0067-0049/210/2/19 , adsurl =

    2014 doi

  83. [98]

    Jour Astron Telescopes, Instruments, and Systems , year = 2015, month = jan, volume = 1, pages =

    Transiting Exoplanet Survey Satellite (TESS). Jour Astron Telescopes, Instruments, and Systems , year = 2015, month = jan, volume = 1, pages =. doi:10.1117/1.JATIS.1.1.014003 , adsurl =

    2015 doi

  84. [99]

    The role of binary separation

    Properties of planets in binary systems. The role of binary separation. A& A , year = 2007, month = jan, volume = 462, pages =. doi:10.1051/0004-6361:20066319 , adsurl =

    2007 doi

  85. [100]

    Nature , year = 2016, month = aug, volume = 536, pages =

    A terrestrial planet candidate in a temperate orbit around Proxima Centauri. Nature , year = 2016, month = aug, volume = 536, pages =. doi:10.1038/nature19106 , adsurl =

    2016 doi

  86. [101]

    A& A , year = 2017, month = feb, volume = 598, pages =

    Proxima's orbit around alpha Centauri. A& A , year = 2017, month = feb, volume = 598, pages =. doi:10.1051/0004-6361/201629930 , adsurl =

    2017 doi

  87. [102]

    Influence of Stellar Multiplicity on Planet Formation. I. Evidence of Suppressed Planet Formation due to Stellar Companions within 20 AU and Validation of Four Planets from the Kepler Multiple Planet Candidates. , year = 2014, month = mar, volume = 783, pages =. doi:10.1088/00...

    2014 doi

  88. [103]

    The Impact of Stellar Multiplicity on Planetary Systems. I. The Ruinous Influence of Close Binary Companions. , year = 2016, month = jul, volume = 152, pages =. doi:10.3847/0004-6256/152/1/8 , adsurl =

    2016 doi

  89. [104]

    Mass accretion and planetary formation in young multiple stellar systems

    GG Tau: the ringworld and beyond. Mass accretion and planetary formation in young multiple stellar systems. A& A Rev , year = 2016, month = jan, volume = 24, pages =. doi:10.1007/s00159-015-0091-5 , adsurl =

    2016 doi

  90. [105]

    , year = 2013, month = may, volume = 431, pages =

    Secular dynamics in hierarchical three-body systems. , year = 2013, month = may, volume = 431, pages =. doi:10.1093/mnras/stt302 , adsurl =

    2013 doi

  91. [106]

    Lett , year = 2005, month = nov, volume = 633, pages =

    Planets in Triple Star Systems: The Case of HD 188753. Lett , year = 2005, month = nov, volume = 633, pages =. doi:10.1086/498302 , adsurl =

    2005 doi

  92. [107]

    , keywords =

    Black Hole Mergers in the Universe. , keywords =. doi:10.1086/312422 , archivePrefix =. astro-ph/9910061 , primaryClass =

    arXiv

  93. [108]

    Suppl Ser , year = 2017, month = apr, volume = 229, pages =

    Revised Stellar Properties of Kepler Targets for the Q1-17 (DR25) Transit Detection Run. Suppl Ser , year = 2017, month = apr, volume = 229, pages =. doi:10.3847/1538-4365/229/2/30 , adsurl =

    2017 doi

  94. [109]

    Planetary Candidates Observed by Kepler. VII. The First Fully Uniform Catalog Based on the Entire 48-month Data Set (Q1-Q17 DR24). Suppl Ser , year = 2016, month = may, volume = 224, pages =. doi:10.3847/0067-0049/224/1/12 , adsurl =

    2016 doi

  95. [110]

    Robo-AO Kepler Survey. IV. The Effect of Nearby Stars on 3857 Planetary Candidate Systems. , year = 2018, month = apr, volume = 155, pages =. doi:10.3847/1538-3881/aab042 , adsurl =

    2018 doi

  96. [111]

    , year = 2017, month = mar, volume = 153, pages =

    Assessing the Effect of Stellar Companions from High-resolution Imaging of Kepler Objects of Interest. , year = 2017, month = mar, volume = 153, pages =. doi:10.3847/1538-3881/153/3/117 , adsurl =

    2017 doi

  97. [112]

    The Kepler Follow-up Observation Program. I. A Catalog of Companions to Kepler Stars from High-Resolution Imaging [ Erratum: 2017AJ....153..201F ]. , year = 2017, month = feb, volume = 153, pages =. doi:10.3847/1538-3881/153/2/71 , adsurl =

    2017 doi

  98. [113]

    , year = 2013, month = jul, volume = 432, pages =

    The dynamical significance of triple star systems in star clusters. , year = 2013, month = jul, volume = 432, pages =. doi:10.1093/mnras/stt617 , adsurl =

    2013 doi

  99. [114]

    , year = 2017, month = may, volume = 467, pages =

    Hypervelocity stars from young stellar clusters in the Galactic Centre. , year = 2017, month = may, volume = 467, pages =. doi:10.1093/mnras/stx106 , adsurl =

    2017 doi

  100. [115]

    , keywords =

    Dynamical origin of S-type planets in close binary stars. , keywords =. 2019. doi:10.1093/mnras/sty3367 , archivePrefix =. 1812.02754 , primaryClass =

    2019 arXiv

  101. [116]

    , year = 2016, month = mar, volume = 456, pages =

    Dynamical formation and scattering of hierarchical triples: cross-sections, Kozai-Lidov oscillations, and collisions. , year = 2016, month = mar, volume = 456, pages =. doi:10.1093/mnras/stv2938 , adsurl =

    2016 doi

  102. [117]

    Planetary Exploration and Science: Recent Results and Advances, Edited by Shuanggen Jin, Nader Haghighipour, and Wing-Huen

    Planet Formation in Binaries. Planetary Exploration and Science: Recent Results and Advances, Edited by Shuanggen Jin, Nader Haghighipour, and Wing-Huen. Springer Geophysics, 309-340 , year = 2015, doi =

    2015

  103. [118]

    , keywords =

    A dynamical origin for planets in triple star systems. , keywords =. 2019. doi:10.1093/mnras/sty3194 , archivePrefix =. 1806.05189 , primaryClass =

    2019 arXiv

  104. [119]

    Calculating the Habitable Zone of Binary Star Systems. I. S-type Binaries. , year = 2013, month = nov, volume = 777, pages =. doi:10.1088/0004-637X/777/2/165 , adsurl =

    2013 doi

  105. [120]

    Exoplanets, Springer Praxis Books

    Formation, Dynamical Evolution, and Habitability of Planets in Binary Star Systems. Exoplanets, Springer Praxis Books. ISBN 978-3-540-74007-0. Praxis Publishing Ltd, Chichester, UK, 2008, p. 223 , year = 2008, doi =

    2008

  106. [121]

    , year = 2007, month = sep, volume = 666, pages =

    Habitable Planet Formation in Binary Planetary Systems. , year = 2007, month = sep, volume = 666, pages =. doi:10.1086/520501 , adsurl =

    2007 doi

  107. [122]

    , year = 2015, month = sep, volume = 452, pages =

    Tidal truncation of inclined circumstellar and circumbinary discs in young stellar binaries. , year = 2015, month = sep, volume = 452, pages =. doi:10.1093/mnras/stv1450 , adsurl =

    2015 doi

  108. [123]

    , year = 2008, month = aug, volume = 388, pages =

    Planet formation in α Centauri A revisited: not so accretion friendly after all. , year = 2008, month = aug, volume = 388, pages =. doi:10.1111/j.1365-2966.2008.13536.x , adsurl =

    2008

  109. [124]

    A& A , year = 2012, month = mar, volume = 539, pages =

    Eccentricity of radiative disks in close binary-star systems. A& A , year = 2012, month = mar, volume = 539, pages =. doi:10.1051/0004-6361/201118075 , adsurl =

    2012 doi

  110. [125]

    Planet Formation in Highly Inclined Binary Systems. I. Planetesimals Jump Inward and Pile Up. , year = 2011, month = jul, volume = 735, pages =. doi:10.1088/0004-637X/735/1/10 , adsurl =

    2011 doi

  111. [126]

    A& A , year = 2010, month = dec, volume = 524, pages =

    Debris discs in binaries: a numerical study. A& A , year = 2010, month = dec, volume = 524, pages =. doi:10.1051/0004-6361/201014851 , adsurl =

    2010 doi

  112. [127]

    , year = 2018, month = aug, volume = 478, pages =

    Formation of S-type planets in close binaries: scattering-induced tidal capture of circumbinary planets. , year = 2018, month = aug, volume = 478, pages =. doi:10.1093/mnras/sty1300 , adsurl =

    2018 doi

  113. [128]

    , year = 2017, month = may, volume = 467, pages =

    Transit probability of precessing circumstellar planets in binaries and exomoons. , year = 2017, month = may, volume = 467, pages =. doi:10.1093/mnras/stx122 , adsurl =

    2017 doi

  114. [129]

    ARAA , year = 2015, month = aug, volume = 53, pages =

    The Occurrence and Architecture of Exoplanetary Systems. ARAA , year = 2015, month = aug, volume = 53, pages =. doi:10.1146/annurev-astro-082214-122246 , adsurl =

    2015 doi

  115. [130]

    , year = 2018, month = nov, volume = 156, pages =

    Properties and Occurrence Rates for Kepler Exoplanet Candidates as a Function of Host Star Metallicity from the DR25 Catalog. , year = 2018, month = nov, volume = 156, pages =. doi:10.3847/1538-3881/aae391 , adsurl =

    2018 doi

  116. [131]

    , year = 2018, month = may, volume = 155, pages =

    Improving the Accuracy of Planet Occurrence Rates from Kepler Using Approximate Bayesian Computation. , year = 2018, month = may, volume = 155, pages =. doi:10.3847/1538-3881/aab9a8 , adsurl =

    2018 doi

  117. [132]

    , year = 2013, month = apr, volume = 766, pages =

    The False Positive Rate of Kepler and the Occurrence of Planets. , year = 2013, month = apr, volume = 766, pages =. doi:10.1088/0004-637X/766/2/81 , adsurl =

    2013 doi

  118. [133]

    , archivePrefix = "arXiv", eprint =

    Young Massive Star Clusters. , archivePrefix = "arXiv", eprint =. doi:10.1146/annurev-astro-081309-130834 , adsurl =

    doi

  119. [134]

    , year = 1996, month = oct, volume = 112, pages =

    A Catalog of Parameters for Globular Clusters in the Milky Way. , year = 1996, month = oct, volume = 112, pages =. doi:10.1086/118116 , adsurl =

    1996 doi

  120. [135]

    A& A , year = 2013, month = aug, volume = 556, pages =

    Three-dimensional modeling of radiative disks in binaries. A& A , year = 2013, month = aug, volume = 556, pages =. doi:10.1051/0004-6361/201321860 , adsurl =

    2013 doi

  121. [136]

    Lett , year = 2000, month = jul, volume = 537, pages =

    Planet Formation is Unlikely in Equal-Mass Binary Systems with A 50 AU. Lett , year = 2000, month = jul, volume = 537, pages =. doi:10.1086/312752 , adsurl =

    2000 doi

  122. [137]

    A& A , year = 2007, month = may, volume = 467, pages =

    Planets in binary systems: is the present configuration indicative of the formation process?. A& A , year = 2007, month = may, volume = 467, pages =. doi:10.1051/0004-6361:20077102 , adsurl =

    2007 doi

  123. [138]

    , keywords =

    Stellar mass-luminosity and mass-radius relations. , keywords =. doi:10.1007/BF00639097 , adsurl =

    doi

  124. [139]

    , keywords =

    Inverse dynamical population synthesis and star formation. , keywords =. 1995. doi:10.1093/mnras/277.4.1491 , archivePrefix =. astro-ph/9508117 , primaryClass =

    1995 arXiv

  125. [140]

    , keywords =

    The dynamical properties of stellar systems in the Galactic disc. , keywords =. 1995. doi:10.1093/mnras/277.4.1507 , archivePrefix =. astro-ph/9508084 , primaryClass =

    1995 arXiv

  126. [141]

    , keywords =

    Dynamical equivalence, the origin of the Galactic field stellar and binary population, and the initial radius-mass relation of embedded clusters. , keywords =. 2018. doi:10.1093/mnras/stx3034 , archivePrefix =. 1711.07987 , primaryClass =

    2018 arXiv

  127. [142]

    , keywords =

    A high binary fraction for the most massive close-in giant planets and brown dwarf desert members. , keywords =. 2019. doi:10.1093/mnras/stz671 , archivePrefix =. 1903.02332 , primaryClass =

    2019 arXiv

  128. [143]

    , keywords =

    Limits on the primordial stellar multiplicity. , keywords =. 2005. doi:10.1051/0004-6361:20052654 , archivePrefix =. astro-ph/0505470 , primaryClass =

    2005 arXiv

  129. [145]

    1995", month =

    A Jupiter-mass companion to a solar-type star. , year = "1995", month = "Nov", volume =. doi:10.1038/378355a0 , adsurl =

    1995 doi

  130. [146]

    Rediscovering Our Galaxy , year = "2018", editor =

    The GOTHAM survey: chemical evolution of Milky Way globular clusters. Rediscovering Our Galaxy , year = "2018", editor =. doi:10.1017/S1743921317007086 , adsurl =

    2018 doi

  131. [147]

    , volume =

    Hughes, Meghan E and Pfeffer, Joel and Martig, Marie and Bastian, Nate and Crain, Robert A and Kruijssen, J M Diederik and Reina-Campos, Marta , title = ". , volume =. 2018 , month =. doi:10.1093/mnras/sty2889 , url =

    2018 doi

  132. [148]

    , keywords =

    Accreted versus in situ Milky Way globular clusters. , keywords =. 2010. doi:10.1111/j.1365-2966.2010.16373.x , archivePrefix =. 1001.4289 , primaryClass =

    2010

  133. [149]

    arXiv e-prints , keywords =

    A galaxy's accretion history unveiled from its integrated spectrum. arXiv e-prints , keywords =. 2019

    2019

  134. [150]

    , keywords =

    Halo mass estimates from the globular cluster populations of 175 low surface brightness galaxies in the Fornax cluster. , keywords =. 2019. doi:10.1093/mnras/stz326 , archivePrefix =. 1901.09648 , primaryClass =

    2019 arXiv

  135. [151]

    , keywords =

    Stars beyond galaxies: the origin of extended luminous haloes around galaxies. , keywords =. 2006. doi:10.1111/j.1365-2966.2005.09789.x , archivePrefix =. astro-ph/0506659 , primaryClass =

    2006

  136. [152]

    , keywords =

    Composition of halo clusters and the formation of the galactic halo. , keywords =. 1978. doi:10.1086/156499 , adsurl =

    1978 doi

  137. [153]

    , keywords =

    Intermediate-mass black holes in binary-rich star clusters. , keywords =. 2019. doi:10.1093/mnras/stz162 , archivePrefix =. 1901.05063 , primaryClass =

    2019 arXiv

  138. [154]

    , keywords =

    Finding black holes with black boxes - using machine learning to identify globular clusters with black hole subsystems. , keywords =. 2019. doi:10.1093/mnras/stz628 , archivePrefix =. 1811.06473 , primaryClass =

    2019 arXiv

  139. [155]

    Relationship to the stellar halo

    The outer halo globular cluster system of M31 - III. Relationship to the stellar halo. , keywords =. 2019. doi:10.1093/mnras/stz072 , adsurl =

    2019 doi

  140. [156]

    , keywords =

    Warp, waves, and wrinkles in the Milky Way. , keywords =. 2018. doi:10.1093/mnras/sty1256 , archivePrefix =. 1712.06616 , primaryClass =

    2018 arXiv

  141. [157]

    , keywords =

    Detecting intermediate-mass ratio inspirals from the ground and space. , keywords =. 2018. doi:10.1103/PhysRevD.98.063018 , archivePrefix =. 1807.03824 , primaryClass =

    2018 arXiv

  142. [158]

    , keywords =

    Very Large Telescope Kinematics for Omega Centauri: Further Support for a Central Black Hole. , keywords =. 2010. doi:10.1088/2041-8205/719/1/L60 , archivePrefix =. 1007.4559 , primaryClass =

    2010 arXiv

  143. [159]

    , keywords =

    A Dynamical N-body model for the central region of Centauri. , keywords =. 2012. doi:10.1051/0004-6361/201116923 , archivePrefix =. 1111.5011 , primaryClass =

    2012 arXiv

  144. [160]

    , keywords =

    N -body modelling of globular clusters: masses, mass-to-light ratios and intermediate-mass black holes. , keywords =. 2017. doi:10.1093/mnras/stw2488 , archivePrefix =. 1609.08794 , primaryClass =

    2017 arXiv

  145. [161]

    , keywords =

    An intermediate-mass black hole in the centre of the globular cluster 47 Tucanae. , keywords =. 2017. doi:10.1038/nature21361 , archivePrefix =. 1702.02149 , primaryClass =

    2017 arXiv

  146. [162]

    , keywords =

    The effect of stellar-mass black holes on the central kinematics of Cen: a cautionary tale for IMBH interpretations. , keywords =. 2019. doi:10.1093/mnras/sty1508 , archivePrefix =. 1806.02157 , primaryClass =

    2019 arXiv

  147. [163]

    , keywords =

    Radial anisotropy in Cen limiting the room for an intermediate-mass black hole. , keywords =. 2017. doi:10.1093/mnras/stx316 , archivePrefix =. 1702.00725 , primaryClass =

    2017 arXiv

  148. [164]

    New Limits on an Intermediate-Mass Black Hole in Omega Centauri. II. Dynamical Models. , keywords =. 2010. doi:10.1088/0004-637X/710/2/1063 , archivePrefix =. 0905.0638 , primaryClass =

    2010 arXiv

  149. [165]

    New Limits on an Intermediate-Mass Black Hole in Omega Centauri. I. Hubble Space Telescope Photometry and Proper Motions. , keywords =. 2010. doi:10.1088/0004-637X/710/2/1032 , archivePrefix =. 0905.0627 , primaryClass =

    2010 arXiv

  150. [166]

    , keywords =

    The Potential of White Dwarf Cosmochronology. , keywords =. 2001. doi:10.1086/319535 , adsurl =

    2001 doi

  151. [167]

    Multi-Object Spectroscopy in the Next Decade: Big Questions, Large Surveys, and Wide Fields , year = "2016", editor =

    Stellar Archaeology with Gaia: The Galactic White Dwarf Population. Multi-Object Spectroscopy in the Next Decade: Big Questions, Large Surveys, and Wide Fields , year = "2016", editor =

    2016

  152. [168]

    , keywords =

    The age of the Milky Way inner halo. , keywords =. 2012. doi:10.1038/nature11062 , archivePrefix =. 1205.6802 , primaryClass =

    2012 arXiv

  153. [169]

    , keywords =

    An independent method for determining the age of the universe. , keywords =. doi:10.1086/184864 , adsurl =

    doi

  154. [170]

    , keywords =

    New results from a survey of faint proper-motion stars - A probable deficiency of very low luminosity degenerates. , keywords =. doi:10.1086/157384 , adsurl =

    doi

  155. [171]

    , year = 1959, month = mar, volume = 129, pages =

    The Rate of Star Formation. , year = 1959, month = mar, volume = 129, pages =. doi:10.1086/146614 , adsurl =

    1959 doi

  156. [172]

    The Cambridge N-Body Lectures , year = 2008, series =

    Initial Conditions for Star Clusters. The Cambridge N-Body Lectures , year = 2008, series =. doi:10.1007/978-1-4020-8431-7_8 , adsurl =. arXiv:0803.1833 , editor =

    2008 arXiv

  157. [173]

    , keywords =

    Multiplicity among M Dwarfs. , keywords =. 1992. doi:10.1086/171708 , adsurl =

    1992 doi

  158. [174]

    IAU Colloq

    CORAVEL Surveys to Study Binaries of Different Masses and Ages. IAU Colloq. 135: Complementary Approaches to Double and Multiple Star Research , year = "1992", editor =

    1992

  159. [175]

    Science , keywords =

    Binary Interaction Dominates the Evolution of Massive Stars. Science , keywords =. 2012. doi:10.1126/science.1223344 , archivePrefix =. 1207.6397 , primaryClass =

    2012 arXiv

  160. [176]

    Active OB Stars: Structure, Evolution, Mass Loss, and Critical Limits , year = "2011", editor =

    The multiplicity of massive stars. Active OB Stars: Structure, Evolution, Mass Loss, and Critical Limits , year = "2011", editor =. doi:10.1017/S1743921311011124 , archivePrefix =. 1009.4197 , primaryClass =

    2011 arXiv

  161. [177]

    , keywords =

    Merging black holes in young star clusters. , keywords =. doi:10.1093/mnras/stz1453 , archivePrefix =. 1901.00863 , primaryClass =

    1901 arXiv

  162. [179]

    arXiv e-prints , keywords =

    Binary black holes in young star clusters: the impact of metallicity. arXiv e-prints , keywords =

  163. [180]

    , keywords =

    On the initial binary population for star cluster simulations. , keywords =. doi:10.1093/mnras/stx1763 , archivePrefix =. 1707.04271 , primaryClass =

    arXiv

  164. [181]

    , keywords =

    Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars. , keywords =. doi:10.3847/1538-4365/aa6fb6 , archivePrefix =. 1606.05347 , primaryClass =

    arXiv

  165. [182]

    , keywords =

    Velocity anisotropy in tidally limited star clusters. , keywords =. doi:10.1093/mnras/stv2574 , archivePrefix =. 1511.02236 , primaryClass =

    arXiv

  166. [183]

    , keywords =

    Kinematical evolution of multiple stellar populations in star clusters. , keywords =. doi:10.1093/mnras/stz1595 , archivePrefix =. 1907.05901 , primaryClass =

    1907 arXiv

  167. [184]

    , keywords =

    Structure and Internal Kinematics of Nine Inner Milky Way Globular Clusters. , keywords =. doi:10.3847/1538-3881/abd036 , archivePrefix =. 2012.00791 , primaryClass =

    2012 arXiv

  168. [185]

    Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Cluster. VI. Improved Data Reduction and Internal-kinematic Analysis of NGC 362. , keywords =. doi:10.3847/1538-4357/aac6c0 , archivePrefix =. 1805.05332 , primaryClass =

    arXiv

  169. [186]

    The HST Large Programme on Centauri. II. Internal Kinematics. , keywords =. doi:10.3847/1538-4357/aaa3ec , archivePrefix =. 1801.01504 , primaryClass =

    arXiv

  170. [187]

    , keywords =

    Deep HST Imaging in 47 Tucanae: A Global Dynamical Model. , keywords =. doi:10.3847/1538-4357/aa974f , archivePrefix =. 1710.10666 , primaryClass =

    arXiv

  171. [188]

    , keywords =

    Self-consistent models of quasi-relaxed rotating stellar systems. , keywords =. doi:10.1051/0004-6361/201118300 , archivePrefix =. 1201.1899 , primaryClass =

    arXiv

  172. [189]

    , keywords =

    Dynamical modelling of globular clusters: challenges for the robust determination of IMBH candidates. , keywords =. doi:10.1093/mnras/staa2821 , archivePrefix =. 2009.07275 , primaryClass =

    2009

  173. [190]

    , keywords =

    Using binaries in globular clusters to catch sight of intermediate-mass black holes. , keywords =. doi:10.1093/mnras/stab2872 , archivePrefix =. 2110.00590 , primaryClass =

    arXiv

  174. [191]

    , keywords =

    No energy equipartition in globular clusters. , keywords =. doi:10.1093/mnras/stt1521 , archivePrefix =. 1302.2152 , primaryClass =

    arXiv

  175. [192]

    AAS/Division of Dynamical Astronomy Meeting \#48 , year = 2017, series =

    New science from the phase space of old stellar systems. AAS/Division of Dynamical Astronomy Meeting \#48 , year = 2017, series =

    2017

  176. [193]

    , keywords =

    Rotating and anisotropic models of globular clusters. , keywords =

  177. [194]

    Galactic Dynamics in the Era of Large Surveys , year = 2020, editor =

    Linear stability of stellar rotating spheres. Galactic Dynamics in the Era of Large Surveys , year = 2020, editor =. doi:10.1017/S1743921319008184 , adsurl =

    2020 doi

  178. [195]

    , keywords =

    Characterization of the velocity anisotropy of accreted globular clusters. , keywords =. doi:10.1093/mnras/stx1680 , archivePrefix =. 1706.09815 , primaryClass =

    arXiv

  179. [196]

    , keywords =

    Globular cluster populations and the kinematical fingerprints of minor mergers. , keywords =. doi:10.1093/mnras/sty2927 , archivePrefix =. 1802.00812 , primaryClass =

    arXiv

  180. [197]

    The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters. XVIII. Proper-motion Kinematics of Multiple Stellar Populations in the Core Regions of NGC 6352. , keywords =. doi:10.3847/1538-4357/ab0551 , archivePrefix =. 1902.02787 , primaryClass =

    arXiv

  181. [198]

    , keywords =

    Radial variation in the stellar mass functions of star clusters. , keywords =. doi:10.1093/mnras/stw2186 , archivePrefix =. 1608.07293 , primaryClass =

    arXiv

  182. [199]

    , keywords =

    On the link between energy equipartition and radial variation in the stellar mass function of star clusters. , keywords =. doi:10.1093/mnras/stw2513 , archivePrefix =. 1609.09082 , primaryClass =

    arXiv

  183. [200]

    , keywords =

    A novel look at energy equipartition in globular clusters. , keywords =. doi:10.1093/mnras/stw552 , archivePrefix =. 1603.00878 , primaryClass =

    arXiv

  184. [201]

    , keywords =

    Kinematic fingerprint of core-collapsed globular clusters. , keywords =. doi:10.1093/mnrasl/sly013 , archivePrefix =. 1801.07781 , primaryClass =

    arXiv

  185. [202]

    Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. IV. Kinematic Profiles and Average Masses of Blue Straggler Stars. , keywords =. doi:10.3847/0004-637X/827/1/12 , archivePrefix =. 1606.00836 , primaryClass =

    arXiv

  186. [203]

    Isolated spherical models with primordial anisotropy

    The kinematic richness of star clusters - I. Isolated spherical models with primordial anisotropy. , keywords =. doi:10.1093/mnras/stx1750 , archivePrefix =. 1707.02792 , primaryClass =

    arXiv

  187. [204]

    , keywords =

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

    2003

  188. [205]

    Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. I. Sample Selection, Data Reduction, and NGC 7078 Results. , keywords =. doi:10.1088/0004-637X/797/2/115 , archivePrefix =. 1410.5820 , primaryClass =

    arXiv

  189. [206]

    Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. V. The Rapid Rotation of 47 Tuc Traced and Modeled in Three Dimensions. , keywords =. doi:10.3847/1538-4357/aa7c5f , archivePrefix =. 1706.08974 , primaryClass =

    arXiv

  190. [207]

    Structure and Dynamics of Disk Galaxies , year = 2014, editor =

    Local Group and Star Cluster Dynamics from HSTPROMO: The Hubble Space Telescope Proper Motion Collaboration. Structure and Dynamics of Disk Galaxies , year = 2014, editor =

    2014

  191. [208]

    Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Cluster. II. Kinematic Profiles and Maps. , keywords =. doi:10.1088/0004-637X/803/1/29 , archivePrefix =. 1502.00005 , primaryClass =

    arXiv

  192. [209]

    , keywords =

    The orbital anisotropy profiles of nearby globular clusters from Gaia Data Release 2. , keywords =. doi:10.1093/mnras/stz1586 , archivePrefix =. 1903.11070 , primaryClass =

    1903 arXiv

  193. [210]

    , keywords =

    Gaia EDR3 view on galactic globular clusters. , keywords =. doi:10.1093/mnras/stab1475 , archivePrefix =. 2102.09568 , primaryClass =

    arXiv

  194. [211]

    Na-O anticorrelation and HB. IX. Kinematics of the program clusters A link between systemic rotation and HB morphology?. , keywords =. doi:10.1051/0004-6361/201118056 , archivePrefix =. 1111.2688 , primaryClass =

    arXiv

  195. [213]

    Unequal masses with a tidal field

    Statistics of N-body simulations - IV. Unequal masses with a tidal field. , keywords =. doi:10.1093/mnras/286.3.709 , adsurl =

    doi

  196. [214]

    Two-component models

    Comparative study between N-body and Fokker-Planck simulations for rotating star clusters - II. Two-component models. , keywords =. doi:10.1093/mnras/stt099 , archivePrefix =. 1211.6527 , primaryClass =

    arXiv

  197. [215]

    , keywords =

    N-body models of rotating globular clusters. , keywords =. doi:10.1111/j.1365-2966.2007.11602.x , archivePrefix =. astro-ph/0702206 , primaryClass =

    2007

  198. [216]

    , keywords =

    Kinematical evolution of tidally limited star clusters: rotational properties. , keywords =. doi:10.1093/mnras/stx853 , archivePrefix =. 1704.05918 , primaryClass =

    arXiv

  199. [217]

    MIKiS: The Multi-instrument Kinematic Survey of Galactic Globular Clusters. I. Velocity Dispersion Profiles and Rotation Signals of 11 Globular Clusters. , keywords =. doi:10.3847/1538-4357/aabe2f , archivePrefix =. 1804.08618 , primaryClass =

    arXiv

  200. [218]

    , keywords =

    A stellar census in globular clusters with MUSE: The contribution of rotation to cluster dynamics studied with 200 000 stars. , keywords =. doi:10.1093/mnras/stx2719 , archivePrefix =. 1710.07257 , primaryClass =

    arXiv

  201. [219]

    MUSE crowded field 3D spectroscopy of over 12 000 stars in the globular cluster NGC 6397. II. Probing the internal dynamics and the presence of a central black hole. , keywords =. doi:10.1051/0004-6361/201527065 , archivePrefix =. 1602.01643 , primaryClass =

    arXiv

  202. [220]

    , keywords =

    The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters: The Internal Kinematics of the Multiple Stellar Populations in NGC 2808. , keywords =. doi:10.1088/2041-8205/810/1/L13 , archivePrefix =. 1508.01804 , primaryClass =

    arXiv

  203. [221]

    Pre-collapse, equal-mass system

    Dynamical evolution of rotating stellar systems - I. Pre-collapse, equal-mass system. , year = 1999, month = jan, volume =. doi:10.1046/j.1365-8711.1999.02083.x , adsurl =

    1999

  204. [222]

    Post-collapse, equal-mass system

    Dynamical evolution of rotating stellar systems - II. Post-collapse, equal-mass system. , keywords =. doi:10.1046/j.1365-8711.2002.05420.x , archivePrefix =. astro-ph/0109062 , primaryClass =

    2002

  205. [223]

    , keywords =

    New insights into star cluster evolution towards energy equipartition. , keywords =. 2021. doi:10.1093/mnrasl/slab026 , archivePrefix =. 2103.06272 , primaryClass =

    2021 arXiv

  206. [224]

    , keywords =

    Evolution towards energy equipartition in star clusters: effects of the tidal field, primordial binaries, and internal velocity anisotropy. , keywords =. 2022. doi:10.1093/mnras/stab3157 , archivePrefix =. 2110.14646 , primaryClass =

    2022 arXiv

  207. [225]

    , keywords =

    Mass segregation and dynamics of primordial binaries in star clusters with a radially anisotropic velocity distribution. , keywords =. doi:10.1093/mnras/stac1776 , archivePrefix =. 2206.11905 , primaryClass =

    arXiv

  208. [226]

    Perturbed stellar motion in dense star clusters

  209. [227]

    On the ambient medium and a stellar association around the supermassive black hole Sagittarius A*

  210. [228]

    Physics Today , keywords =

    How a fake Kepler portrait became iconic. Physics Today , keywords =. doi:10.1063/PT.3.4825 , archivePrefix =. 2108.02213 , primaryClass =

    arXiv

  211. [229]

    , keywords =

    Dissipationless galaxy formation and the R to the 1/4-power law. , keywords =. doi:10.1093/mnras/201.4.939 , adsurl =

    doi

  212. [230]

    , keywords =

    Unexpected formation modes of the first hard binary in core collapse. , keywords =. doi:10.1016/j.newast.2011.09.001 , archivePrefix =. 1107.3866 , primaryClass =

    2011 arXiv

  213. [231]

    Astronomy and Computing , keywords =

    Few-body modes of binary formation in core collapse. Astronomy and Computing , keywords =. doi:10.1016/j.ascom.2013.11.002 , archivePrefix =. 1208.4131 , primaryClass =

    2013 arXiv

  214. [232]

    Star Cluster Evolution with Primordial Binaries. I. A Comparative Study. , keywords =. doi:10.1086/169289 , adsurl =

    doi

  215. [233]

    Star Cluster Evolution with Primordial Binaries. II. Detailed Analysis. , keywords =. doi:10.1086/169958 , adsurl =

    doi

  216. [234]

    Star Cluster Evolution with Primordial Binaries. III. Effect of the Galactic Tidal Field. , keywords =. doi:10.1086/174186 , adsurl =

    doi

  217. [235]

    , keywords =

    On equipartition of kinetic energies in two-component star clusters. , keywords =

  218. [236]

    , keywords =

    Two-component stellar systems in thermal and dynamical equilibrium. , keywords =. doi:10.1086/112891 , adsurl =

    doi

  219. [237]

    Pisma v Astronomicheskii Zhurnal , keywords =

    Spherical systems of gravitating bodies with ellipsoidal velocity distribution. Pisma v Astronomicheskii Zhurnal , keywords =

  220. [238]

    , keywords =

    Spherical stellar systems with spheroidal velocity distributions. , keywords =. doi:10.1086/113810 , adsurl =

    doi

  221. [239]

    Classical and Quantum Gravity , keywords =

    Loss-cone dynamics. Classical and Quantum Gravity , keywords =. doi:10.1088/0264-9381/30/24/244005 , archivePrefix =. 1307.3268 , primaryClass =

    arXiv

  222. [240]

    , keywords =

    An analytic inversion for anisotropic spherical galaxies. , keywords =. doi:10.1093/mnras/253.3.414 , adsurl =

    doi

  223. [241]

    A family of models of partially relaxed stellar systems. II. Comparison with the products of collisionless collapse. , keywords =. doi:10.1051/0004-6361:20041705 , archivePrefix =. astro-ph/0411541 , primaryClass =

    arXiv

  224. [242]

    Dynamical evolution of models in a tidal field

    Star clusters with primordial binaries - II. Dynamical evolution of models in a tidal field. , keywords =. doi:10.1111/j.1365-2966.2006.11166.x , archivePrefix =. astro-ph/0602409 , primaryClass =

    2006

  225. [243]

    , keywords =

    Kinematical fingerprints of star cluster early dynamical evolution. , keywords =. doi:10.1093/mnrasl/slu088 , archivePrefix =. 1406.3634 , primaryClass =

    arXiv

  226. [244]

    , keywords =

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

    arXiv

  227. [245]

    , keywords =

    Statistics of N-Body Simulations - Part Two - Equal Masses after Core Collapse. , keywords =. doi:10.1093/mnras/270.2.298 , archivePrefix =. astro-ph/9403024 , primaryClass =

    arXiv

  228. [246]

    Unequal masses

    Statistics of N-body simulations - III. Unequal masses. , keywords =. doi:10.1093/mnras/279.3.1037 , archivePrefix =. astro-ph/9506143 , primaryClass =

    arXiv

  229. [247]

    , keywords =

    Three-component Kinematics of Multiple Stellar Populations in Globular Clusters with Gaia and VLT. , keywords =. doi:10.3847/1538-4357/ab5aee , archivePrefix =. 1905.09908 , primaryClass =

    1905 arXiv

  230. [248]

    , keywords =

    Monte Carlo simulations of multiple populations in globular clusters: constraints on the cooling flow versus accretion scenario using million bodies simulations. , keywords =. doi:10.1093/mnras/stab154 , archivePrefix =. 2102.01707 , primaryClass =

    arXiv

  231. [249]

    , keywords =

    The internal rotation of globular clusters revealed by Gaia DR2. , keywords =. doi:10.1093/mnras/sty2365 , archivePrefix =. 1806.02580 , primaryClass =

    arXiv

  232. [250]

    , keywords =

    The eye of Gaia on globular clusters kinematics: internal rotation. , keywords =. doi:10.1093/mnras/stz505 , archivePrefix =. 1902.05895 , primaryClass =

    1902 arXiv

  233. [251]

    , keywords =

    Binary evolution in stellar dynamics. , keywords =. doi:10.1093/mnras/173.3.729 , adsurl =

    doi

  234. [252]

    Random Gravitational Encounters and the Evolution of Spherical Systems. III. Halo. , year = 1972, month = may, volume =. doi:10.1086/151442 , adsurl =

    1972 doi

  235. [253]

    , year = 1968, month = jan, volume =

    The gravo-thermal catastrophe in isothermal spheres and the onset of red-giant structure for stellar systems. , year = 1968, month = jan, volume =. doi:10.1093/mnras/138.4.495 , adsurl =

    1968 doi

  236. [254]

    , keywords =

    Astrophysical and dark matter interpretations of extended gamma-ray emission from the Galactic Center. , keywords =. doi:10.1103/PhysRevD.90.023526 , archivePrefix =. 1402.4090 , primaryClass =

    arXiv

  237. [255]

    , keywords =

    A tale of tails: Dark matter interpretations of the Fermi GeV excess in light of background model systematics. , keywords =. doi:10.1103/PhysRevD.91.063003 , archivePrefix =. 1411.4647 , primaryClass =

    arXiv

  238. [256]

    , keywords =

    Millisecond Pulsars and the Gamma-Ray Excess in Andromeda. , keywords =. doi:10.3847/2041-8213/aafc62 , archivePrefix =. 1808.02497 , primaryClass =

    arXiv

  239. [257]

    JCAP , keywords =

    Distinguishing dark matter from unresolved point sources in the Inner Galaxy with photon statistics. JCAP , keywords =. doi:10.1088/1475-7516/2015/05/056 , archivePrefix =. 1412.6099 , primaryClass =

    2015 arXiv

  240. [258]

    , keywords =

    Strong Support for the Millisecond Pulsar Origin of the Galactic Center GeV Excess. , keywords =. doi:10.1103/PhysRevLett.116.051102 , archivePrefix =. 1506.05104 , primaryClass =

    arXiv

  241. [259]

    , keywords =

    The Fermi Galactic Center GeV Excess and Implications for Dark Matter. , keywords =. doi:10.3847/1538-4357/aa6cab , archivePrefix =. 1704.03910 , primaryClass =

    arXiv

  242. [260]

    , keywords =

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

    arXiv

  243. [261]

    , keywords =

    On black hole subsystems in idealized nuclear star clusters. , keywords =. doi:10.1093/mnras/stt1599 , archivePrefix =. 1308.4641 , primaryClass =

    arXiv

  244. [262]

    Black hole-black hole binaries

    Dynamics of stellar black holes in young star clusters with different metallicities - II. Black hole-black hole binaries. , keywords =. doi:10.1093/mnras/stu824 , archivePrefix =. 1404.7147 , primaryClass =

    arXiv

  245. [263]

    , keywords =

    Close encounters with the Death Star: Interactions between collapsed bodies and the Solar System. , keywords =. doi:10.1051/0004-6361/202140454 , archivePrefix =. 2103.12745 , primaryClass =

    arXiv

  246. [264]

    1969", month =

    Equipartition and the Formation of Compact Nuclei in Spherical Stellar Systems. , year = "1969", month = "Dec", volume =. doi:10.1086/180451 , adsurl =

    1969 doi

  247. [265]

    , keywords =

    A necessary condition for equilibrium in stellar systems with a continuous mass spectrum. , keywords =. doi:10.1086/156332 , adsurl =

    doi

  248. [266]

    , keywords =

    A planetary system around the millisecond pulsar PSR1257 + 12. , keywords =. doi:10.1038/355145a0 , adsurl =

    doi

  249. [267]

    , keywords =

    A debris disk around an isolated young neutron star. , keywords =. doi:10.1038/nature04669 , archivePrefix =. astro-ph/0604076 , primaryClass =

    arXiv

  250. [268]

    IAU Colloq

    Orbital Parameters of the PSR B1620-26 Triple System. IAU Colloq. 160: Pulsars: Problems and Progress , year = 1996, editor =

    1996

  251. [269]

    , keywords =

    The dynamical fate of planetary systems in young star clusters. , keywords =. doi:10.1093/mnras/stv1832 , archivePrefix =. 1508.01593 , primaryClass =

    arXiv

  252. [270]

    , keywords =

    Dynamics of Planetary Systems in Star Clusters. , keywords =. doi:10.1088/0004-637X/697/1/458 , archivePrefix =. astro-ph/0612757 , primaryClass =

    arXiv

  253. [271]

    , keywords =

    Stability of multiplanetary systems in star clusters. , keywords =. doi:10.1093/mnras/stx1464 , archivePrefix =. 1706.03789 , primaryClass =

    arXiv

  254. [272]

    , keywords =

    The dynamical evolution of multiplanet systems in open clusters. , keywords =. doi:10.1093/mnras/stt771 , archivePrefix =. 1305.1413 , primaryClass =

    arXiv

  255. [273]

    , keywords =

    Dynamical Interactions Make Hot Jupiters in Open Star Clusters. , keywords =. doi:10.3847/0004-637X/816/2/59 , archivePrefix =. 1411.7061 , primaryClass =

    arXiv

  256. [274]

    , archivePrefix = "arXiv", eprint =

    The Galactic distribution of X-ray binaries and its implications for compact object formation and natal kicks. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stx027 , adsurl =

    doi

  257. [275]

    , eprint =

    How Black Holes Get Their Kicks: Gravitational Radiation Recoil Revisited. , eprint =. doi:10.1086/421552 , adsurl =

    doi

  258. [277]

    , eprint =

    The pulsar kick velocity distribution. , eprint =. doi:10.1093/mnras/291.3.569 , adsurl =

    doi

  259. [278]

    , eprint =

    The distances to Galactic low-mass X-ray binaries: consequences for black hole luminosities and kicks. , eprint =. doi:10.1111/j.1365-2966.2004.08193.x , adsurl =

    2004

  260. [279]

    , year = 2018, month = jan, volume = 473, pages =

    Probing the formation history of the nuclear star cluster at the Galactic Centre with millisecond pulsars. , year = 2018, month = jan, volume = 473, pages =. doi:10.1093/mnras/stx2364 , adsurl =

    2018 doi

  261. [280]

    , year = 2018, month = apr, volume = 475, pages =

    Disrupted globular clusters and the gamma-ray excess in the Galactic Centre. , year = 2018, month = apr, volume = 475, pages =. doi:10.1093/mnras/sty183 , adsurl =

    2018 doi

  262. [281]

    , year = 2015, month = oct, volume = 812, pages =

    Disrupted Globular Clusters Can Explain the Galactic Center Gamma-Ray Excess. , year = 2015, month = oct, volume = 812, pages =. doi:10.1088/0004-637X/812/1/15 , adsurl =

    2015 doi

  263. [282]

    , keywords =

    Wang, Long and Iwasawa, Masaki and Nitadori, Keigo and Makino, Junichiro , doi =. , keywords =. arXiv , arxivId =:2006.16560 , issn =

    2006 arXiv

  264. [283]

    Environmental Effects on the Dynamical Evolution of Star Clusters in Turbulent Molecular Clouds

  265. [284]

    , keywords =

    Environmental effects on the dynamical evolution of star clusters in turbulent molecular clouds. , keywords =. doi:10.1051/0004-6361/202243579 , archivePrefix =. 2207.01634 , primaryClass =

    arXiv

  266. [285]

    , keywords =

    MOCCA-SURVEY Database I: Binary black hole mergers from globular clusters with intermediate mass black holes. , keywords =. doi:10.1093/mnras/staa2677 , archivePrefix =. 2008.10823 , primaryClass =

    2008 arXiv

  267. [286]

    , keywords =

    MOCCA-SURVEY data base II - Properties of intermediate mass black holes escaping from star clusters. , keywords =. doi:10.1093/mnras/stac1728 , archivePrefix =. 2111.09223 , primaryClass =

    arXiv

  268. [288]

    , keywords =

    The effect of pair-instability mass loss on black-hole mergers. , keywords =. doi:10.1051/0004-6361/201628980 , archivePrefix =. 1607.03116 , primaryClass =

    arXiv

  269. [289]

    , keywords =

    Pulsational Pair-instability Supernovae. , keywords =. doi:10.3847/1538-4357/836/2/244 , archivePrefix =. 1608.08939 , primaryClass =

    arXiv

  270. [290]

    , keywords =

    The Pair-instability Mass Gap for Black Holes. , keywords =. doi:10.3847/2041-8213/abf2c4 , archivePrefix =. 2103.07933 , primaryClass =

    arXiv

  271. [291]

    , year = 1994, month = may, volume = 369, pages =

    High birth velocities of radio pulsars. , year = 1994, month = may, volume = 369, pages =. doi:10.1038/369127a0 , adsurl =

    1994 doi

  272. [292]

    , archivePrefix = "arXiv", eprint =

    A stellar-mass black hole population in the globular cluster NGC 6101?. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stw1726 , adsurl =

    doi

  273. [293]

    Clues on the initial mass function and black hole retention fraction

    The global mass functions of 35 Galactic globular clusters - II. Clues on the initial mass function and black hole retention fraction. , keywords =. doi:10.1093/mnras/stx2036 , archivePrefix =. 1708.09530 , primaryClass =

    arXiv

  274. [294]

    , archivePrefix = "arXiv", eprint =

    Compact Binary Merger Rates: Comparison with LIGO/Virgo Upper Limits. , archivePrefix = "arXiv", eprint =. doi:10.3847/0004-637X/819/2/108 , adsurl =

    doi

  275. [295]

    , keywords =

    Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction. , keywords =. doi:10.1051/0004-6361/201629685 , adsurl =

    doi

  276. [296]

    , keywords =

    Presupernova evolution in massive interacting binaries. , keywords =. doi:10.1086/171341 , adsurl =

    doi

  277. [297]

    , eprint =

    The galactic evolution of the supernova rates. , eprint =. doi:10.1016/S1384-1076(03)00069-1 , adsurl =

    doi

  278. [298]

    , keywords =

    Preparing the next gravitational million-body simulations: evolution of single and binary stars in NBODY6++GPU, MOCCA, and MCLUSTER. , keywords =. doi:10.1093/mnras/stab3748 , archivePrefix =. 2105.08067 , primaryClass =

    arXiv

  279. [299]

    , year = 1990, month = feb, volume =

    Duplicity of Hot Helium Subdwarfs. , year = 1990, month = feb, volume =

    1990

  280. [300]

    , keywords =

    The unseen population of F- to K-type companions to hot subdwarf stars. , keywords =. doi:10.1111/j.1365-2966.2012.21415.x , archivePrefix =. 1205.6803 , primaryClass =

    2012

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.