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Journal articles on the topic 'Star cluster formation and evolution'

Author: Grafiati

Published: 10 March 2023

Last updated: 31 July 2025

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1

Kroupa, Pavel. "Star-cluster formation and evolution." Proceedings of the International Astronomical Union 2, S237 (2006): 230–37. http://dx.doi.org/10.1017/s1743921307001524.

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AbstractStar clusters are observed to form in a highly compact state and with low star-formation efficiencies, and only 10 per cent of all clusters appear to survive to middle- and old-dynamical age. If the residual gas is expelled on a dynamical time the clusters disrupt. Massive clusters may then feed a hot kinematical stellar component into their host-galaxy's field population thereby thickening galactic disks, a process that theories of galaxy formation and evolution need to accommodate. If the gas-evacuation time-scale depends on cluster mass, then a power-law embedded-cluster mass functi

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Parmentier, Geneviève. "Early dynamical evolution of star cluster systems." Proceedings of the International Astronomical Union 5, S266 (2009): 87–94. http://dx.doi.org/10.1017/s1743921309990913.

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AbstractViolent relaxation, the protocluster dynamical response to the expulsion of its residual star-forming gas, is a short albeit crucial episode in the evolution of star clusters and star cluster systems. Because it is heavily driven by cluster-formation and environmental conditions, it is a potentially highly rewarding phase in terms of probing star formation and galaxy evolution. In this contribution, I review how cluster-formation and environmental conditions affect the shape of the young cluster mass function and the relation between the present star-formation rate of galaxies and the

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Vesperini, Enrico. "Star cluster dynamics." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 368, no. 1913 (2010): 829–49. http://dx.doi.org/10.1098/rsta.2009.0260.

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Dynamical evolution plays a key role in shaping the current properties of star clusters and star cluster systems. A detailed understanding of the effects of evolutionary processes is essential to be able to disentangle the properties that result from dynamical evolution from those imprinted at the time of cluster formation. In this review, I focus my attention on globular clusters, and review the main physical ingredients driving their early and long-term evolution, describe the possible evolutionary routes and show how cluster structure and stellar content are affected by dynamical evolution.

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Ishchenko, M., V. Masliukh, M. Hradov, P. Berczik, B. Shukirgaliyev, and C. Omarov. "Dynamical evolution of the open clusters with different star formation efficiencies and orbital parameters." Astronomy & Astrophysics 694 (January 30, 2025): A33. https://doi.org/10.1051/0004-6361/202452336.

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Context. Open star clusters are dynamic systems whose evolution is critically influenced by initial conditions such as star formation efficiency and orbital parameters. Understanding their dissolution mechanisms provides insight into stellar population dynamical mixing in the Milky Way. Aims. We aim to investigate the dynamical evolution and dissolution of initially non-virialised open clusters by examining how different global star formation efficiencies and orbital characteristics impact the cluster longevity and structural changes. We followed the evolution of the clusters up to their disso

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Zepf, Stephen E. "The Formation and Evolution of Star Clusters and Galaxies." Highlights of Astronomy 13 (2005): 347–49. http://dx.doi.org/10.1017/s1539299600015938.

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AbstractThis paper addresses the questions of what we have learned about how and when dense star clusters form, and what studies of star clusters have revealed about galaxy formation and evolution. One important observation is that globular clusters are observed to form in galaxy mergers and starbursts in the local universe, which both provides constraints on models of globular cluster formation, and suggests that similar physical conditions existed when most early-type galaxies and their globular clusters formed in the past. A second important observation is that globular cluster systems typi

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Gieles, Mark. "Star cluster disruption." Proceedings of the International Astronomical Union 5, S266 (2009): 69–80. http://dx.doi.org/10.1017/s1743921309990895.

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AbstractStar clusters are often used as tracers of major star-formation events in external galaxies as they can be studied out to much greater distances than individual stars. It is vital to understand their evolution if they are used to derive, for example, the star-formation history of their host galaxy. More specifically, we want to know how cluster lifetimes depend on their environment and on structural properties such as mass and radius. This review presents a theoretical overview of the early evolution of star clusters and the consequent long-term survival chances. It is suggested that c

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Anders, Peter, Uta Fritze –. v. Alvensleben, and Richard de Grijs. "Young Star Clusters: Progenitors of Globular Clusters!?" Highlights of Astronomy 13 (2005): 366–68. http://dx.doi.org/10.1017/s1539299600015987.

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AbstractStar cluster formation is a major mode of star formation in the extreme conditions of interacting galaxies and violent starbursts. Young clusters are observed to form in a variety of such galaxies, a substantial number resembling the progenitors of globular clusters in mass and size, but with significantly enhanced metallicity. From studies of the metal-poor and metal-rich star cluster populations of galaxies, we can therefore learn about the violent star formation history of these galaxies, and eventually about galaxy formation and evolution. We present a new set of evolutionary synth

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Clarke, C. J. "Star Formation in Large N Clusters." Symposium - International Astronomical Union 207 (2002): 489–98. http://dx.doi.org/10.1017/s0074180900224297.

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We focus here on the gas dynamics of cluster formation and the early stellar dynamical evolution of young clusters. We point out that the condition that a cloud can fragment into a large number of pieces places rather particular constraints on its initial state; we also review the processes that shape the stellar IMF in cluster formation simulations. We show how N-body calculations and observations can be combined to discover the properties of clusters at the point at which they first become stellar dynamical (as opposed to gas dynamical systems). Finally, we touch on the question of how proto

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Fensch, Jérémy, Pierre-Alain Duc, Médéric Boquien, et al. "Massive star cluster formation and evolution in tidal dwarf galaxies." Astronomy & Astrophysics 628 (August 2019): A60. http://dx.doi.org/10.1051/0004-6361/201834403.

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Context. The formation of globular clusters remains an open debate. Dwarf starburst galaxies are efficient at forming young massive clusters with similar masses as globular clusters and may hold the key to understanding their formation. Aims. We study star cluster formation in a tidal debris, including the vicinity of three tidal dwarf galaxies, in a massive gas-dominated collisional ring around NGC 5291. These dwarfs have physical parameters that differ significantly from local starbursting dwarfs. They are gas rich, highly turbulent, their gas metallicity is already enriched up to half solar

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Lee, Seong-Kook, Myungshin Im, Eunhee Ko, et al. "Star-formation Property of High Redshift Galaxies in Clusters: Perceptive View from Observation and Simulation." Proceedings of the International Astronomical Union 17, S373 (2021): 260–63. http://dx.doi.org/10.1017/s1743921322004409.

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AbstractThe evolution of star formation properties of galaxies depends on the environment where galaxies reside, and generally star formation of galaxies in dense environment decreases more quickly. Interestingly, the star formation property of high-redshift galaxies clusters vary largely even though they are at similar redshift. We have found that the large-scale environment surrounding each galaxy cluster can contribute to make this cluster-by-cluster variation. This correlation is found in the results from observational data as well as in the simulations of galaxy formation. We suggest the

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Randriamanakoto, Zara, and Petri Väisänen. "Young massive clusters in Arp 299." Proceedings of the International Astronomical Union 14, S351 (2019): 143–46. http://dx.doi.org/10.1017/s1743921319007701.

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AbstractBecause of their young ages and compact densities, young massive star clusters (YMCs) are widely considered as potential proto-globular clusters. They are ubiquitous in environments with ongoing star formation activity such as interacting luminous infrared galaxies. To determine the galactic environmental effects on the star cluster formation and evolution, we study the YMC population of Arp 299 (NGC 3690E/NGC 3690W) using data taken with the HST WFC3/UVIS camera. By fitting the multiband photometry with the Yggdrasil models, we derive the star cluster masses, ages and extinction. Whil

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Lada, Charles J. "The physics and modes of star cluster formation: observations." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 368, no. 1913 (2010): 713–31. http://dx.doi.org/10.1098/rsta.2009.0264.

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Stellar clusters are born in cold and dusty molecular clouds and the youngest clusters are embedded to various degrees in a dusty dark molecular material. Such embedded clusters can be considered protocluster systems. The most deeply buried examples are so heavily obscured by dust that they are only visible at infrared wavelengths. These embedded protoclusters constitute the nearest laboratories for a direct astronomical investigation of the physical processes of cluster formation and early evolution. I review the present state of empirical knowledge concerning embedded-cluster systems and dis

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Baumgardt, H., and P. Kroupa. "The Influence of Gas Expulsion on the Evolution of Star Clusters." Proceedings of the International Astronomical Union 3, S246 (2007): 36–40. http://dx.doi.org/10.1017/s1743921308015238.

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AbstractWe present new results on the dynamical evolution and dissolution of star clusters due to residual gas expulsion and the effect this has on the mass function and other properties of star cluster systems. To this end, we have carried out a large set of N-body simulations, varying the star formation efficiency, gas expulsion time scale and strength of the external tidal field, obtaining a three-dimensional grid of models which can be used to predict the evolution of individual star clusters or whole star cluster systems by interpolating between our runs. When applied to the Milky Way glo

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Cournoyer-Cloutier, Claude, Alison Sills, William E. Harris, et al. "Massive Star Cluster Formation with Binaries. I. Evolution of Binary Populations." Astrophysical Journal 977, no. 2 (2024): 203. https://doi.org/10.3847/1538-4357/ad90b3.

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Abstract We study the evolution of populations of binary stars within massive cluster-forming regions. We simulate the formation of young massive star clusters within giant molecular clouds with masses ranging from 2 × 104 to 3.2 × 105 M ⊙. We use Torch, which couples stellar dynamics, magnetohydrodynamics, star and binary formation, stellar evolution, and stellar feedback through the Amuse framework. We find that the binary fraction decreases during cluster formation at all molecular cloud masses. The binaries’ orbital properties also change, with stronger and quicker changes in denser, more

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Grijs, Richard de. "“Super” Star Clusters." Highlights of Astronomy 13 (2005): 363–65. http://dx.doi.org/10.1017/s1539299600015975.

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AbstractThe production of “super star clusters” (SSCs; luminous, compact star clusters) seems to be a hallmark of intense star formation, particularly in interacting and star-burst galaxies. Their sizes, luminosities, and mass estimates are entirely consistent with what is expected for young Milky Way-type globular clusters (GCs). SSCs are important because of what they can tell us about GC formation and evolution (e.g., initial characteristics and early survival rates). They are also of prime importance as probes of the formation and (chemical) evolution of their host galaxies, and of the ini

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Karam, Jeremy, Michiko S. Fujii, and Alison Sills. "Dynamics of Star Cluster Formation: The Effects of Ongoing Star Formation and Stellar Feedback." Astrophysical Journal 984, no. 1 (2025): 75. https://doi.org/10.3847/1538-4357/adc719.

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Abstract We perform a high-resolution zoomed-in simulation of star cluster assembly including the merger of two subclusters with initial conditions taken from previous large-scale giant molecular cloud (GMC) simulations. We couple hydrodynamics to N-body dynamics to simulate the individual stars themselves, and the gas-rich environment in which they evolve. We include prescriptions for star formation and stellar feedback and compare them directly to previous simulations of the same region without these prescriptions to determine their role in shaping the dynamics inherited from the cluster ass

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Assmann, P., M. Fellhauer, and M. I. Wilkinson. "Star clusters as building blocks for dSph galaxy formation." Proceedings of the International Astronomical Union 5, S266 (2009): 353–56. http://dx.doi.org/10.1017/s174392130999127x.

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AbstractWe study numerically the formation of dSph galaxies. Intense starbursts, e.g., in gas-rich environments, typically produce a few to a few hundred young star clusters within a region of just a few hundred pc. The dynamical evolution of these star clusters may explain the formation of the luminous component of dwarf spheroidal (dSph) galaxies. Here, we perform a numerical experiment to show that the evolution of star cluster complexes in dark-matter haloes can explain the formation of the luminous components of dSph galaxies.

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Santiago, Basílio X. "The star clusters of the Magellanic System." Proceedings of the International Astronomical Union 4, S256 (2008): 69–80. http://dx.doi.org/10.1017/s1743921308028287.

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AbstractMore than 50 years have elapsed since the first studies of star clusters in the Magellanic Clouds. The wealth of data accumulated since then has not only revealed a large cluster system, but also a diversified one, filling loci in the age, mass and chemical abundance parameter space which are complementary to Galactic clusters. Catalogs and photometric samples currently available cover most of the cluster mass range. The expectations of relatively long cluster disruption timescales in the Clouds have been confirmed, allowing reliable assessments of the cluster initial mass function and

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Smith, R., J. I. Davies, and A. Nelson. "Tidal Influences on Cluster Dwarf Evolution." Proceedings of the International Astronomical Union 3, S244 (2007): 378–80. http://dx.doi.org/10.1017/s1743921307014366.

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AbstractUsing N-Body/Treecode, SPH simulations, including a self regulating Star Formation-feedback model, the influence of cluster tidal forces on infalling dwarf irregulars is investigated. Results suggest that an encounter with the cluster potential can disrupt a rotating disk causing morphological transformation of the gaseous component, resulting in an enhancement of star formation rates (SFRs) of up to an order of magnitude.

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Carraro, Giovanni, Richard de Grijs, Bruce Elmegreen, et al. "HIGHLIGHTS OF COMMISSION 37 SCIENCE RESULTS." Proceedings of the International Astronomical Union 11, T29A (2015): 502–21. http://dx.doi.org/10.1017/s174392131600096x.

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AbstractIt is widely accepted that stars do not form in isolation but result from the fragmentation of molecular clouds, which in turn leads to star cluster formation. Over time, clusters dissolve or are destroyed by interactions with molecular clouds or tidal stripping, and their members become part of the general field population. Star clusters are thus among the basic building blocks of galaxies. In turn, star cluster populations, from young associations and open clusters to old globulars, are powerful tracers of the formation, assembly, and evolutionary history of their parent galaxies. Al

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Baumgardt, Holger, Junichiro Makino, and Simon Portegies Zwart. "Formation and Evolution of Massive Black Holes in Star Clusters." Highlights of Astronomy 13 (2005): 350–53. http://dx.doi.org/10.1017/s153929960001594x.

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AbstractWe present results of N-body simulations on the formation of massive black holes by run-away merging in young star clusters and the later dynamical evolution of star clusters containing massive black holes. We determine the initial conditions necessary for run-away merging to form a massive black hole and study the equilibrium profile that is established in the cluster center as a result of the interaction of stars with the central black hole. Our results show that star clusters which contain black holes have projected luminosity profiles that can be fitted by standard King models. The

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Randriamanakoto, Zara, and Petri Väisänen. "The SUNBIRD survey: characterizing the super star cluster populations of intensely star-forming galaxies." Proceedings of the International Astronomical Union 12, S316 (2015): 70–76. http://dx.doi.org/10.1017/s1743921315010510.

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AbstractSuper star clusters (SSCs) represent the youngest and most massive form of known gravitationally bound star clusters in the Universe. They are born abundantly in environments that trigger strong and violent star formation. We investigate the properties of these massive SSCs in a sample of 42 nearby starbursts and luminous infrared galaxies. The targets form the sample of the SUperNovae and starBursts in the InfraReD (SUNBIRD) survey that were imaged using near-infrared (NIR) K-band adaptive optics mounted on the Gemini/NIRI and the VLT/NaCo instruments. Results from i) the fitted power

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Kodama, Tadayuki, Masao Hayashi, Yusei Koyama, Ken-ichi Tadaki, Ichi Tanaka, and Rhythm Shimakawa. "Mahalo-Subaru: Mapping Star Formation at the Peak Epoch of Massive Galaxy Formation." Proceedings of the International Astronomical Union 8, S295 (2012): 74–77. http://dx.doi.org/10.1017/s1743921313004353.

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AbstractMAHALO-Subaru (MApping HAlpha and Lines of Oxygen with Subaru) is our on-going large programme which aims to investigate how the star forming activities in galaxies are propagated as a function of time, mass, and environment. We are targeting 10 clusters and proto-clusters at 0.4<z<2.6, and two general fields (GOODS-N and SXDF-CANDELS) with Suprime-Cam and MOIRCS by utilizing our unique sets of narrow-band filters. The narrow-band imaging can map out star forming galaxies with the redshifted Halpha and/or [OII] emission lines from our targets, and thus providing relatively unbias

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Webb, Jeremy J., and Alison Sills. "The initial properties of young star clusters in M83." Monthly Notices of the Royal Astronomical Society 501, no. 2 (2020): 1933–39. http://dx.doi.org/10.1093/mnras/staa3832.

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ABSTRACT The initial sizes and masses of massive star clusters provide information about the cluster formation process and also determine how cluster populations are modified and destroyed, which have implications for using clusters as tracers of galaxy assembly. Young massive cluster populations are often assumed to be unchanged since cluster formation; therefore, their distributions of masses and radii are used as the initial values. However, the first few hundred million years of cluster evolution does change both cluster mass and cluster radius, through both internal and external processes

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de Grijs, Richard. "A revolution in star cluster research: setting the scene." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 368, no. 1913 (2010): 693–711. http://dx.doi.org/10.1098/rsta.2009.0253.

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Star clusters and their stellar populations play a significant role in the context of galaxy evolution, across space (from local to high redshift) and time (from currently forming to fossil remnants). We are now within reach of answering a number of fundamental questions that will have a significant impact on our understanding of key open issues in contemporary astrophysics, ranging from the formation, assembly and evolution of galaxies to the details of the star-formation process. Our improved understanding of the physics driving star cluster formation and evolution has led to the emergence o

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Sabbi, Elena, Linda J. Smith, Lynn R. Carlson, et al. "Time resolved star formation in the SMC: the youngest star clusters." Proceedings of the International Astronomical Union 4, S256 (2008): 244–49. http://dx.doi.org/10.1017/s1743921308028512.

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AbstractThe two young clusters NGC 346 and NGC 602 in the Small Magellanic Cloud provide us with the opportunity to study and the efficiency of feedback mechanism at low metallicity, as well as the impact of local and global conditions in cluster formation and evolution. I describe the latest results from a multi-wavelength, large-scale study of these two clusters. HST/ACS images reveal that the clusters have very different structures: NGC 346 is composed by a number of sub-clusters which appear coeval with ages of 3 ± 1 Myr, strongly suggesting formation by the hierarchical fragmentation of a

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Portegies Zwart, Simon F. "The formation of intermediate mass black holes." Symposium - International Astronomical Union 208 (2003): 145–56. http://dx.doi.org/10.1017/s0074180900207109.

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We study the growth rate of stars in dense star clusters by stellar collisions. Our analytic calculations are in good agreement with direct N-body simulations with up to 65536 stars performed on the GRAPE family of computers. We find that star clusters with a half mass relaxation time ≲ 20 Myr are dominated by stellar collisions. The first collision occurs at the moment of core collapse. The collision dominated phase last until the cluster dissolves in the tidal field of the Galaxy or mass loss by stellar evolution arrests core collapse. The majority of collisions occur with the same star resu

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Anders, Peter, Uta Fritze-V. Alvensleben, and Richard de Grijs. "Young Star Clusters: Clues to Galaxy Formation and Evolution." Symposium - International Astronomical Union 217 (2004): 210–11. http://dx.doi.org/10.1017/s0074180900197529.

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Young clusters are observed to form in a variety of interacting galaxies and violent starbursts, a substantial number resembling the progenitors of the well-studied globular clusters in mass and size. By studying young clusters in merger remnants and peculiar galaxies, we can therefore learn about the violent star formation history of these galaxies. We present a new set of evolutionary synthesis models of our GALEV code specifically developed to include the gaseous emission of presently forming star clusters, and a new tool that allows to determine individual cluster metallicities, ages, exti

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Harris, William E. "Young, old, massive: Steps to understanding globular cluster formation." Proceedings of the International Astronomical Union 14, S351 (2019): 3–12. http://dx.doi.org/10.1017/s1743921319006495.

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AbstractOn observational grounds we now know a huge amount about the characteristics of massive star clusters in galaxies of all types, from the smallest dwarfs to the most massive giants and even into the Intracluster Medium. The old globular clusters (GCs) in particular exhibit a high degree of uniformity across all these environments in their physical properties including scale size, luminosity distribution, metallicity distribution, and age. As survivors of a long period of dynamical evolution, they are “unusual, but not special” among star clusters.The past few years have seen major advan

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Adamo, Angela. "The Imprints Of Galactic Environment On Cluster Formation and Evolution." Proceedings of the International Astronomical Union 12, S316 (2015): 17–24. http://dx.doi.org/10.1017/s1743921315010571.

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AbstractYoung star clusters (YSCs) appear to be a ubiquitous product of star formation in local galaxies, thus, they can be used to study the star formation process at work in their host galaxies. Moreover, YSCs are intrinsically brighter that single stars, potentially becoming the most important tracers of the recent star formation history in galaxies in the local Universe. In local galaxies, we also witness the presence of a large population of evolved star clusters, commonly called globular clusters (GCs). GCs peak formation history is very close to the redshift (z ~ 2) when the cosmic star

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Shukirgaliyev, Bekdaulet, Genevieve Parmentier, Peter Berczik, and Andreas Just. "Star Clusters in the Galactic tidal field, from birth to dissolution." Proceedings of the International Astronomical Union 14, S351 (2019): 507–11. http://dx.doi.org/10.1017/s1743921319006781.

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AbstractWe study the evolution of star clusters in the Galactic tidal field starting from their birth in molecular clumps. Our model clusters form according to the local-density-driven cluster formation model in which the stellar density profile is steeper than that of gas. As a result, clusters resist the gas expulsion better than predicted by earlier models.We vary the impact of the Galactic tidal field λ, considering different Galactocentric distances (3-18 kpc), as well as different cluster sizes. Our model clusters survive the gas expulsion independent of λ.We investigated the relation be

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Román-Zúñiga, Carlos G., Elizabeth A. Lada, and Bruno Ferreira. "A Near-infrared Survey of the Rosette Complex: Clues of Early Cluster Evolution." Proceedings of the International Astronomical Union 3, S246 (2007): 46–49. http://dx.doi.org/10.1017/s1743921308015251.

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AbstractThe majority of stars in our galaxy are born in embedded clusters, which can be considered the fundamental units of star formation. We have recently surveyed the star forming content of the Rosette Complex using FLAMINGOS in order to investigate the properties of its embedded clusters. We discuss the results of our near-infrared imaging survey. In particular, we on the first evidence for the early evolution and expansion of the embedded clusters. In addition we present data suggesting a temporal sequence of cluster formation across the cloud and discuss the influence of the HII region

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Konstantopoulos, I. S., N. Bastian, M. Gieles, and H. J. G. L. M. Lamers. "Constraining star cluster disruption mechanisms." Proceedings of the International Astronomical Union 5, S266 (2009): 433–37. http://dx.doi.org/10.1017/s1743921309991621.

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AbstractStar clusters are found in all sorts of environments, and their formation and evolution is inextricably linked to the star-formation process. Their eventual destruction can result from a number of factors at different times, but the process can be investigated as a whole through the study of cluster age distributions. Observations of populous cluster samples reveal a distribution following a power law of index approximately −1. In this work, we use M33 as a test case to examine the age distribution of an archetypal cluster population and show that it is, in fact, the evolving shape of

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Pérez-Martínez, J. M., B. Ziegler, A. Böhm, and M. Verdugo. "Galaxy kinematics across different environments in the RXJ1347−1145 cluster complex." Astronomy & Astrophysics 637 (May 2020): A30. http://dx.doi.org/10.1051/0004-6361/201936243.

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Aims. In order to understand the role of the different processes that drive galaxy evolution in clusters, we need comprehensive studies that simultaneously examine several of the most important physical properties of galaxies. In this work we study the interplay between the kinematic state and star formation activity of galaxies in the RXJ1347−1145 cluster complex at z ∼ 0.45. Methods. We used VLT/VIMOS to obtain slit spectra for 95 galaxies across the 40′ × 40′ area where the RXJ1347−1145 cluster complex resides. We determined the cluster membership of our targets by identifying one or more o

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Fall, S. Michael, and Qing Zhang. "Formation and Disruption of Globular Star Clusters." Symposium - International Astronomical Union 207 (2002): 566–76. http://dx.doi.org/10.1017/s0074180900224388.

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In the first part of this article, we review observations of the mass and luminosity functions of young and old star cluster systems. We also review some of the physical processes that may determine the characteristic mass of globular clusters and the form of their mass function. In the second part of this article, we summarize our models for the disruption of clusters and the corresponding evolution of the mass function. Much of our focus here is on understanding why the mass function of globular clusters has no more than a weak dependence on radius within their host galaxies.

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Li, Hui, and Oleg Gnedin. "Formation and evolution of globular clusters in cosmological simulations." Proceedings of the International Astronomical Union 14, S351 (2019): 34–39. http://dx.doi.org/10.1017/s1743921319007646.

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AbstractIn a series of three papers, we introduced a novel cluster formation model that describes the formation, growth, and disruption of star clusters in high-resolution cosmological simulations. We tested this model on a Milky Way-sized galaxy and found that various properties of young massive clusters, such as the mass function and formation efficiency, are consistent with observations in the local universe. Interestingly, most massive clusters – globular cluster candidates – are preferentially formed during major merger events. We follow the dynamical evolution of clusters in the galactic

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Obidowski, Justine C., Jeremy J. Webb, Simon Portegies Zwart, and Maxwell X. Cai. "Oort Cloud Formation and Evolution in Star Clusters." Astrophysical Journal 987, no. 1 (2025): 29. https://doi.org/10.3847/1538-4357/add92c.

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Abstract It is unknown whether an Oort cloud reaches its maximum mass within its star’s birth cluster or millions of years later. Complicating the Oort cloud evolution process is the fact that comets can be stripped from orbit due to perturbations from passing stars. We explore how a star’s cluster escape time (t esc) and the time its Oort cloud reaches maximum mass (t max ) affect the Oort cloud’s ability to survive via N-body simulations. In a 14 M ⊙ pc–3 cluster, we identify 50 stars of 1 M ⊙ with a range of t esc to host Oort clouds, each with 1000 comets at t max . For each host, we consi

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Decressin, T. "Formation of globular clusters with multiple populations." Proceedings of the International Astronomical Union 12, S316 (2015): 281–86. http://dx.doi.org/10.1017/s1743921315010613.

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AbstractSpectroscopic and photometric evidences have led to a complete revision of our understanding of globular clusters with the discovery of multiple stellar populations which differ chemically. Whereas some stars have a chemical composition similar to fields stars, others show large star-to-star variations in light elements (Li to Al) while their composition in iron and heavy elements stay constant. This peculiar chemical pattern can be explained by self-pollution of the intracluster gas occurring in the early evolution of clusters. Here the possible impact from a first generation of fast

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Belczynski, K., A. Askar, M. Arca-Sedda, et al. "The origin of the first neutron star – neutron star merger." Astronomy & Astrophysics 615 (July 2018): A91. http://dx.doi.org/10.1051/0004-6361/201732428.

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The first neutron star-neutron star (NS-NS) merger was discovered on August 17, 2017 through gravitational waves (GW170817) and followed with electromagnetic observations. This merger was detected in an old elliptical galaxy with no recent star formation. We perform a suite of numerical calculations to understand the formation mechanism of this merger. We probe three leading formation mechanisms of double compact objects: classical isolated binary star evolution, dynamical evolution in globular clusters, and nuclear cluster formation to test whether they are likely to produce NS-NS mergers in

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Bekki, Kenji. "Star cluster dynamics in galaxies." Proceedings of the International Astronomical Union 5, S266 (2009): 219–30. http://dx.doi.org/10.1017/s1743921309991086.

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AbstractI present a review of star cluster (SC) dynamics in galaxies, with special emphasis on the effects of global galactic dynamics on SC formation and evolution. I particularly discuss (i) dynamical friction processes affecting SCs in galaxies of different masses, (ii) formation of stellar galactic nuclei and massive globular clusters (GCs) through multiple merging of SCs, (iii) interactions between giant molecular clouds (GMCs) and SCs, (iv) SC destruction due to the strong tidal fields in galaxy mergers and (v) the formation of low-mass dwarfs from numerous SCs. I also discuss some recen

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Olsen, K. A. G., P. W. Hodge, M. Mateo, et al. "Results from HST Observations of Six LMC Globular Cluster Fields." Symposium - International Astronomical Union 190 (1999): 448–49. http://dx.doi.org/10.1017/s0074180900118534.

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We present deep HST color-magnitude diagrams of fields centered on the six old LMC globular clusters NGC 1754, NGC 1835, NGC 1898, NGC 1916, NGC 2005, and NGC 2019. Separate cluster and field star CMDs are shown. The time of formation of the LMC is studied from an analysis of the cluster CMDs. Based on a comparison of the CMDs with sequences of the Milky Way clusters M3, M5, and M55, we suggest that the LMC formed its first stars at the same time as the Milky Way to within 1 Gyr. We find additional evidence that these LMC globular clusters are as old as the oldest Milky Way clusters through a

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Grudić, Michael Y., J. M. Diederik Kruijssen, Claude-André Faucher-Giguère, et al. "A model for the formation of stellar associations and clusters from giant molecular clouds." Monthly Notices of the Royal Astronomical Society 506, no. 3 (2021): 3239–58. http://dx.doi.org/10.1093/mnras/stab1894.

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ABSTRACT We present a large suite of magnetohydrodynamic simulations of turbulent, star-forming giant molecular clouds (GMCs) with stellar feedback, extending previous work by simulating 10 different random realizations for each point in the parameter space of cloud mass and size. It is found that once the clouds disperse due to stellar feedback, both self-gravitating star clusters and unbound stars generally remain, which arise from the same underlying continuum of substructured stellar density, i.e. the hierarchical cluster formation scenario. The fraction of stars that are born within gravi

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Gouliermis, Dimitrios A., and Sacha Hony. "NGC 346: Looking in the Cradle of a Massive Star Cluster." Proceedings of the International Astronomical Union 12, S316 (2015): 117–22. http://dx.doi.org/10.1017/s1743921316008759.

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AbstractHow does a star cluster of more than few 10,000 solar masses form? We present the case of the cluster NGC 346 in the Small Magellanic Cloud, still embedded in its natal star-forming region N66, and we propose a scenario for its formation, based on observations of the rich stellar populations in the region. Young massive clusters host a high fraction of early-type stars, indicating an extremely high star formation efficiency. The Milky Way galaxy hosts several young massive clusters that fill the gap between young low-mass open clusters and old massive globular clusters. Only a handful,

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Reina-Campos, Marta, Oleg Y. Gnedin, Alison Sills, and Hui Li. "The Star Clusters as Links between Galaxy Evolution and Star Formation Project. I. Numerical Method." Astrophysical Journal 978, no. 1 (2024): 15. https://doi.org/10.3847/1538-4357/ad909f.

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Abstract Stellar clusters are critical constituents within galaxies: They are the result of highest-density star formation, and through their spatially and temporally correlated feedback, they regulate their host galaxy evolution. We present a novel numerical method to model star clusters as individual units of star formation using sink particles. In our method, star clusters grow via gas accretion and via merging with less massive clusters. We describe the implementation in the radiation hydrodynamics code GIZMO and run a large grid of marginally bound, turbulent clouds of 107 M ⊙ to explore

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Tan, Jonathan C., Suzanne N. Shaske, and Sven Van Loo. "Molecular Clouds: Internal Properties, Turbulence, Star Formation and Feedback." Proceedings of the International Astronomical Union 8, S292 (2012): 19–28. http://dx.doi.org/10.1017/s1743921313000173.

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AbstractAll stars are born in molecular clouds, and most in giant molecular clouds (GMCs), which thus set the star formation activity of galaxies. We first review their observed properties, including measures of mass surface density, Σ, and thus mass,M. We discuss cloud dynamics, concluding most GMCs are gravitationally bound. Star formation is highly clustered within GMCs, but overall is very inefficient. We compare properties of star-forming clumps with those of young stellar clusters (YSCs). The high central densities of YSCs may result via dynamical evolution of already-formed stars during

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Chatterjee, Sourav, Meagan Morscher, Carl L. Rodriguez, Bharat Pattabiraman, and Frederic A. Rasio. "Effects of Stellar-Mass Black Holes on Massive Star Cluster Evolution." Proceedings of the International Astronomical Union 12, S316 (2015): 234–39. http://dx.doi.org/10.1017/s1743921315010674.

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AbstractRecent observations have revealed the existence of stellar mass black hole (BH) candidates in some globular clusters (GC) in the Milky Way and in other galaxies. Given that the detection of BHs is challenging, these detections likely indicate the existence of large populations of BHs in these clusters. This is in direct contrast to the past understanding that at most a handful of BHs may remain in old GCs due to quick mass segregation and rapid mutual dynamical ejection. Modern realistic star-by-star numerical simulations suggest that the retention fraction of BHs is typically much hig

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Kruijssen, J. M. Diederik. "Are globular clusters the natural outcome of regular high-redshift star formation?" Proceedings of the International Astronomical Union 10, S312 (2014): 147–54. http://dx.doi.org/10.1017/s1743921315007759.

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AbstractWe summarise the recent progress in understanding the formation and evolution of globular clusters (GCs) in the context of galaxy formation and evolution. It is discussed that an end-to-end model for GC formation and evolution should capture four different phases: (1) star and cluster formation in the high-pressure interstellar medium of high-redshift galaxies, (2) cluster disruption by tidal shocks in the gas-rich host galaxy disc, (3) cluster migration into the galaxy halo, and (4) the final evaporation-dominated evolution of GCs until the present day. Previous models have mainly foc

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Whitmore, Bradley C. "The Evolution of Young Star Clusters in Merging Galaxies." Symposium - International Astronomical Union 186 (1999): 251–60. http://dx.doi.org/10.1017/s0074180900112719.

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The formation of young star clusters in merging galaxies is, by now, well established. The new challenge is to use these young clusters as a tool to address some of the outstanding questions. For example, what fraction of these young clusters become globular clusters? Is this enough to explain the difference in the specific globular cluster frequencies for spirals and ellipticals? What is it about the collision between two gas-rich galaxies that triggers giant molecular clouds to form star clusters? Can the star clusters be used to age date merger remnants and establish a convincing evolutiona

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Kumamoto, Jun, Michiko S. Fujii, and Ataru Tanikawa. "Merger rate density of binary black holes formed in open clusters." Monthly Notices of the Royal Astronomical Society 495, no. 4 (2020): 4268–78. http://dx.doi.org/10.1093/mnras/staa1440.

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ABSTRACT Several binary black holes (BBHs) have been observed using gravitational wave detectors. For the formation mechanism of BBHs, two main mechanisms, isolated binary evolution and dynamical formation in dense star clusters, have been suggested. Future observations are expected to provide more information about BBH distributions, and it will help us to distinguish the two formation mechanisms. For the star cluster channel, globular clusters have mainly been investigated. However, recent simulations have suggested that BBH formation in open clusters is not negligible. We estimate a local m

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Venuti, L., L. Prisinzano, G. G. Sacco, et al. "The Gaia-ESO Survey and CSI 2264: Substructures, disks, and sequential star formation in the young open cluster NGC 2264." Astronomy & Astrophysics 609 (December 22, 2017): A10. http://dx.doi.org/10.1051/0004-6361/201731103.

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Context. Reconstructing the structure and history of young clusters is pivotal to understanding the mechanisms and timescales of early stellar evolution and planet formation. Recent studies suggest that star clusters often exhibit a hierarchical structure, possibly resulting from several star formation episodes occurring sequentially rather than a monolithic cloud collapse. Aims. We aim to explore the structure of the open cluster and star-forming region NGC 2264 (~3 Myr), which is one of the youngest, richest and most accessible star clusters in the local spiral arm of our Galaxy; we link the

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