Relevant bibliographies by topics / Star cluster

Academic literature on the topic 'Star cluster'

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Published: 4 June 2021
Last updated: 8 June 2024

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Journal articles on the topic "Star cluster"

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Vesperini, Enrico. "Star cluster dynamics." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 368, no. 1913 (February 28, 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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Palouš, Jan, Richard Wünsch, Guillermo Tenorio-Tagle, and Sergyi Silich. "Origin of Star-to-Star Abundance Inhomogeneities in Star Clusters." Proceedings of the International Astronomical Union 4, S254 (June 2008): 233–38. http://dx.doi.org/10.1017/s1743921308027646.

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AbstractThe mass reinserted by young stars of an emerging massive compact cluster shows a bimodal hydrodynamic behaviour. In the inner part of the cluster, it is thermally unstable, while in its outer parts it forms an out-blowing wind. The chemical homogeneity/inhomogeneity of low/high mass clusters demonstrates the relevance of this solution to the presence of single/multiple stellar populations. We show the consequences that the thermal instability of the reinserted mass has to the galactic super-winds.
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Gieles, Mark. "Star cluster disruption." Proceedings of the International Astronomical Union 5, S266 (August 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 clusters forming with initial densities of ≳104 M⊙ pc−3 survive the gas expulsion, or ‘infant mortality,’ phase. At ~10Myr, they are bound and have densities of ~103±1 M⊙ pc−3. After this time, they are stable against expansion through stellar evolution, encounters with giant molecular clouds and will most likely survive for another Hubble time if they are located in a moderate tidal field. Clusters with lower initial densities (≲100 M⊙ pc−3) will disperse into the field within a few 10s of Myrs. Some discussion is given on how extragalactic star cluster populations, and especially their age distributions, can be used to gain insight into disruption.
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Turner, D. G. "Are the Cepheids in Cluster Nuclei a Rare Breed?" International Astronomical Union Colloquium 82 (1985): 209–11. http://dx.doi.org/10.1017/s0252921100109340.

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As reviewed by Kholopov (1968), star counts for a variety of open clusters reveal the existence of low density coronal regions surrounding the nuclear concentrations of most star clusters. Such cluster coronae have diameters 2.5 to 5 times larger than the respective nuclear diameters for clusters which are poor to medium-rich in member stars, and have star densities only about 10% those observed in cluster nuclei. Cluster coronae therefore contain roughly 40% to 70% of the stars in an open cluster, and are subsequently a (or, more appropriately, the) major component of most star clusters.
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Kroupa, Pavel. "Star-cluster formation and evolution." Proceedings of the International Astronomical Union 2, S237 (August 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 function may transform within a few dozen Myr to a mass function with a turnover near 105M, thereby possibly explaining this universal empirical feature. Discordant empirical evidence on the mass function of star clusters leads to the insight that the physical processes shaping early cluster evolution remain an issue of cutting-edge research.
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Fujii, Michiko S. "Inter-cluster velocity structures of star cluster complexes." Proceedings of the International Astronomical Union 14, S351 (May 2019): 197–99. http://dx.doi.org/10.1017/s1743921319007634.

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AbstractStar clusters are often born as star-cluster systems, which include several stellar clumps. Such star-cluster complexes could have formed from turbulent molecular clouds. Since Gaia Data Release 2 provided us high quality velocity data of individual stars in known star-cluster complexes, we now can compare the velocity structures of the observed star-cluster complexes with simulated ones. We performed a series of N-body simulations for the formation of star-cluster complexes starting from turbulent molecular clouds. We measured the inter-cluster velocity dispersions of our simulated star-cluster complexes and compared them with the Carina region and NGC 2264. We found that the Carina region and NGC 2264 formed from molecular clouds with a mass of ∼4 × 105M⊙ and ∼4 × 104M⊙, respectively. In our simulations, we also found that the maximum cluster mass (Mc,max) in the complex follows ${M_{{\rm{c}},{\rm{max}}}} = 0.{\rm{2}}0M_g^{0.76}$, where Mg is the initial gas mass.
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Larsen, Søren S. "Open, Massive and Globular Clusters — Part of the Same Family?" Symposium - International Astronomical Union 207 (2002): 421–27. http://dx.doi.org/10.1017/s0074180900224133.

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Populations of young star clusters show significant differences even among “normal” disk galaxies. In this contribution I discuss how properties of young cluster systems are related to those of their host galaxies, based on a recent study of clusters in a sample of 22 nearby spiral galaxies. Luminous young clusters similar to the “super” star clusters observed in starbursts and mergers exist in several of these galaxies, and it is found that the luminosity of the brightest star cluster as well as the specific luminosity of the cluster systems both correlate well with the host galaxy star formation rate. When considering star clusters in different environments the traditional distinction between “open”, “massive” and “globular” clusters breaks down, underscoring the need for a universal physical description of cluster formation.
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Fujii, M., M. Iwasawa, Y. Funato, and J. Makino. "Fully Self-Consistent N-body Simulation of Star Cluster in the Galactic Center." Proceedings of the International Astronomical Union 3, S246 (September 2007): 467–68. http://dx.doi.org/10.1017/s1743921308016177.

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AbstractWe have developed a new tree-direct hybrid algorithm, “Bridge”. It can simulate small scale systems embedded within large-N systems fully self-consistently. Using this algorithm, we have performed full N-body simulations of star clusters near the Galactic center (GC) and compared the orbital evolutions of the star cluster with those obtained by “traditional” simulations, in which the orbital evolution of the star clusters is calculated from the dynamical friction formula. We found that the inspiral timescale of the star cluster is shorter than that obtained with traditional simulations. Moreover, we investigated the eccentricities of particles escaped from the star cluster. Eccentric orbit of the star cluster can naturally explain the high eccentricities of the observed stars.
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Hurley, Jarrod R., Michael M. Shara, and Christopher A. Tout. "Star Clusters as Exotic Star Factories." International Astronomical Union Colloquium 187 (2002): 115–20. http://dx.doi.org/10.1017/s0252921100001305.

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AbstractIn light of recent N-body simulations performed using the GRAPE-6 special-purpose hardware we discuss the role of the star cluster environment in producing unusual stellar populations and the possibility that stars labelled exotic in the solar neighbourhood may be commonplace within star clusters.
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Da Costa, G. S. "Star Clusters in the Magellanic Clouds." Symposium - International Astronomical Union 190 (1999): 397–404. http://dx.doi.org/10.1017/s0074180900118406.

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Recent results for the old and intermediate-age star clusters of the Magellanic Clouds are reviewed. Highlights include new evidence that the LMC old clusters are as old the Galaxy's halo globular clusters and the persistence of the LMC cluster “Age Gap” despite field star evidence for significant star formation during the cluster age gap epoch. For the SMC new data confirm the lack of significant change in cluster abundances with age prior to ~4 Gyr ago.
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Dissertations / Theses on the topic "Star cluster"

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Dale, J. E. "Feedback in star cluster formation." Thesis, University of Cambridge, 2004. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.598249.

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Massive stars emit strong fluxes of ionising radiation and their dynamical impact on their natal clusters is expected to be severe. The outflows generated expel residual gas from the cluster and can potentially gravitationally disrupt it. The loss of its reserves of molecular gas also prevents the cluster forming more stars. Star-formation and star cluster evolution cannot be fully understood without a proper treatment of feedback. I present a novel technique I have developed to allow the inclusion of the effects of ionising radiation in smoothed particle hydrodynamics (SPH) simulations of star clusters. The new algorithm is able to reproduce the results of simple analytical models and also gives results in good agreement with a more sophisticated Monte Carlo radiative transfer code when tested under highly anisotropic conditions. I simulate the effects of ionising radiation in globular clusters and compare my results with one-dimensional calculations with which I find good agreement. I investigate three cases in which different quantities of gas are distributed in my model cluster such that the as becomes fully ionised either during the HII region’s formation phase, or during its expansion phase, or such that the HII region is trapped inside the cluster core. I find gas expulsion to be quite efficient in the calculations in which the HII region escapes the core. I observe an instability in the second calculation which causes the shocked shell driven by the ionisation front to fragment as the HII region exits the core. The instability produces new structure from the smooth gas in the system, but this structure is rapidly destroyed by the radiation field and the effect of the instability on the evolution of the system is minimal. I also simulate feedback in the context of young embedded clusters, a highly inhomogeneous and anisotropic environment. I find that, again, photoionisation is able to produce novel structure in the ambient gas, causing it to fragment into filaments and beads. This fragmentation of the neutral gas, together with compression by hot ionised gas, which decreases the Jeans mass, lead me to conclude that feedback promotes star formation.
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Adamo, A., J. E. Ryon, M. Messa, H. Kim, K. Grasha, D. O. Cook, D. Calzetti, et al. "Legacy ExtraGalactic UV Survey with The Hubble Space Telescope: Stellar Cluster Catalogs and First Insights Into Cluster Formation and Evolution in NGC 628." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624449.

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We report the large effort that is producing comprehensive high-level young star cluster (YSC) catalogs for a significant fraction of galaxies observed with the Legacy ExtraGalactic UV Survey (LEGUS) Hubble treasury program. We present the methodology developed to extract cluster positions, verify their genuine nature, produce multiband photometry (from NUV to NIR), and derive their physical properties via spectral energy distribution fitting analyses. We use the nearby spiral galaxy NGC 628 as a test case for demonstrating the impact that LEGUS will have on our understanding of the formation and evolution of YSCs and compact stellar associations within their host galaxy. Our analysis of the cluster luminosity function from the UV to the NIR finds a steepening at the bright end and at all wavelengths suggesting a dearth of luminous clusters. The cluster mass function of NGC 628 is consistent with a power-law distribution of slopes similar to-2 and a truncation of a few times 10(5) M-circle dot. After their formation, YSCs and compact associations follow different evolutionary paths. YSCs survive for a longer time frame, confirming their being potentially bound systems. Associations disappear on timescales comparable to hierarchically organized star-forming regions, suggesting that they are expanding systems. We find massindependent cluster disruption in the inner region of NGC 628, while in the outer part of the galaxy there is little or no disruption. We observe faster disruption rates for low mass (<= 10(4) M-circle dot) clusters, suggesting that a massdependent component is necessary to fully describe the YSC disruption process in NGC 628.
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Breen, Philip Gavin. "Dynamical evolution of idealised star cluster models." Thesis, University of Edinburgh, 2013. http://hdl.handle.net/1842/8296.

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This thesis is concerned with the dynamical evolution of globular star clusters modelled as the classical gravitational N-body problem. The models in this thesis are idealised in order to allow the detailed study of particular dynamical aspects of the cluster evolution. Examples of properties which tend to be omitted are stellar evolution, primordial binaries and the effect of an external tidal gravitational field. The methods used in this thesis are gas models, N-body models and physical arguments. One of the main topics in this thesis is gravothermal oscillations in multicomponent star clusters. The evolution of one-component globular clusters, systems with equal particle masses, is quite well understood. However, the evolution of more realistic globular clusters, with a range of particle masses, is a much more complicated matter. The condition for the on-set of gravothermal oscillations in a one-component system is simply that the number of stars is greater than a certain number ( ≈7000). In a multi-component system the relationship between the number of stars at which the gravothermal oscillations first appear and the stellar mass distribution of a cluster is a complex one. In order to investigate this phenomenon two different types of multi-component systems were studied: two-component systems (the simplest approximation of a mass spectrum, Chapter 2) and ten-component systems (which were realisations of continuous power law IMFs, Chapter 3). In both cases the critical number of stars at which gravothermal oscillations first appear are found empirically for a range of stellar mass distributions. The nature of the oscillations themselves are investigated and it is shown that the oscillations can be understood by focusing on the behaviour of the heavier stars within the cluster. A parameter Nef (de nined Mtot/mmax where Mtot is the total mass and mmax is the maximum stellar mass) acts as an approximate stability boundary for multicomponent systems.The stability boundary was found to be at Nef ~- 12000. In this Chapter 4, globular star clusters which contain a sub-system of stellar-mass black holes (BH) are investigated. This is done by considering two-component models, as these are the simplest approximation of more realistic multi-mass systems, where one component represents the BH population and the other represents all the other stars. These systems are found to undergo a long phase of evolution where the centre of the system is dominated by a BH sub-system. After mass segregation has driven most of the BH into a compact sub-system, the evolution of the BH sub-system is found to be in uenced by the cluster in which it is contained. The BH sub-system evolves in such a way as to satisfy the energy demands of the whole cluster, just as the core of a one component system must satisfies the energy demands of the whole cluster. The BH sub-system is found to exist for a significant amount of time. It takes approximately 10trh;i, where trh;i is the initial half-mass relaxation time, from the formation of the compact BH sub-system up until the time when 90% of the sub-system total mass is lost (which is of order 103 times the half-mass relaxation time of the BH sub-system at its time of formation). Based on theoretical arguments the rate of mass loss from the BH sub-system (M2) is predicted to be (βζM)/(αtrh): where M is the total mass, trh is the half-mass relaxation time, and α, β, ζ are three dimensionless parameters. (see Section 4.3 for details). An interesting consequence of this is that the rate of mass loss from the BH sub-system is approximately independent of the stellar mass ratio (m2/m1) and the total mass ratio (M2/M1) (in the range m2/m1 ≥ 10 and M2/M1 ≈ 10-2, where m1, m2 are the masses of individual low-mass and high-mass particles respectively, and M1, M2 are the corresponding total mass). The theory is found to be in reasonable agreement with most of the results of a series of N-body simulations, and all of the models if the value of ζ is suitable adjusted. Predictions based on theoretical arguments are also made about the structure of BH sub-systems. Other aspects of the evolution are also considered such as the conditions for the onset of gravothermal oscillation. The final chapter (Chapter 5) of the thesis contains some concluding comments as well as a discussion on some possible future projects, for which the results in this thesis would be useful.
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Pozzo, Monica. "The effect of high-mass stars on low-mass star formation." Thesis, Keele University, 2001. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.366445.

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Randriamanakoto, Rojovola Zara-Nomena. "Super star cluster candidates in the star-forming regions of luminous infrared galaxies." Master's thesis, University of Cape Town, 2010. http://hdl.handle.net/11427/11807.

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We report on a study of super star cluster (SSC) candidates in the star-forming regions of a representative sample of local luminous infrared galaxies (LIRGs) using KS-band near-infrared (NIR) adaptive optics imaging with GEMINI/ALTAIR and VLT/NACO instruments. The evolution of the cosmic star formation rate (CSFR) indicates its rapid decline in the local Universe.
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Canning, Rebecca Elizabeth Ann. "Star and filament formation in brightest cluster galaxies." Thesis, University of Cambridge, 2012. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.610523.

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Santoro, Fernando. "Semi analytical simulations of primordial star cluster formation." Thesis, University of Sussex, 2003. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.288843.

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Simanton, Lesley Ann. "Star Cluster Populations in the Spiral Galaxy M101." University of Toledo / OhioLINK, 2015. http://rave.ohiolink.edu/etdc/view?acc_num=toledo1437587267.

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Harris, William E., Stephanie M. Ciccone, Gwendolyn M. Eadie, Oleg Y. Gnedin, Douglas Geisler, Barry Rothberg, and Jeremy Bailin. "GLOBULAR CLUSTER SYSTEMS IN BRIGHTEST CLUSTER GALAXIES. III. BEYOND BIMODALITY." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/622870.

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We present new deep photometry of the rich globular cluster (GC) systems around the Brightest Cluster Galaxies UGC 9799 (Abell 2052) and UGC 10143 (Abell 2147), obtained with the Hubble Space Telescope (HST) ACS and WFC3 cameras. For comparison, we also present new reductions of similar HST/ACS data for the Coma supergiants NGC 4874 and 4889. All four of these galaxies have huge cluster populations (to the radial limits of our data, comprising from 12,000 to 23,000 clusters per galaxy). The metallicity distribution functions (MDFs) of the GCs can still be matched by a bimodal-Gaussian form where the metal-rich and metal-poor modes are separated by similar or equal to 0.8 dex, but the internal dispersions of each mode are so large that the total MDF becomes very broad and nearly continuous from [Fe/H] similar or equal to-2.4 to solar. There are, however, significant differences between galaxies in the relative numbers of metal-rich clusters, suggesting that they underwent significantly different histories of mergers with massive gas-rich halos. Last, the proportion of metal-poor GCs rises especially rapidly outside projected radii R >= 4 R-eff, suggesting the importance of accreted dwarf satellites in the outer halo. Comprehensive models for the formation of GCs as part of the hierarchical formation of their parent galaxies will be needed to trace the systematic change in structure of the MDF with galaxy mass, from the distinctly bimodal form in smaller galaxies up to the broad continuum that we see in the very largest systems.
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Messa, M., A. Adamo, G. Östlin, D. Calzetti, K. Grasha, E. K. Grebel, F. Shabani, et al. "The young star cluster population of M51 with LEGUS – I. A comprehensive study of cluster formation and evolution." OXFORD UNIV PRESS, 2018. http://hdl.handle.net/10150/626277.

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Recently acquired WFC3 UV (F275W and F336W) imaging mosaics under the Legacy Extragalactic UV Survey (LEGUS), combined with archival ACS data of M51, are used to study the young star cluster (YSC) population of this interacting system. Our newly extracted source catalogue contains 2834 cluster candidates, morphologically classified to be compact and uniform in colour, for which ages, masses and extinction are derived. In this first work we study the main properties of the YSC population of the whole galaxy, considering a mass-limited sample. Both luminosity and mass functions follow a power-law shape with slope -2, but at high luminosities and masses a dearth of sources is observed. The analysis of the mass function suggests that it is best fitted by a Schechter function with slope -2 and a truncation mass at 1.00 +/- 0.12 x 10(5) M-circle dot . Through Monte Carlo simulations, we confirm this result and link the shape of the luminosity function to the presence of a truncation in the mass function. A mass limited age function analysis, between 10 and 200 Myr, suggests that the cluster population is undergoing only moderate disruption. We observe little variation in the shape of the mass function at masses above 1 x 10(4) M-circle dot over this age range. The fraction of star formation happening in the form of bound clusters in M51 is similar to 20 per cent in the age range 10-100 Myr and little variation is observed over the whole range from 1 to 200 Myr.
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Books on the topic "Star cluster"

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F, Prosser Charles, and United States. National Aeronautics and Space Administration., eds. An X-ray survey of the open cluster NGC 6475 (M7) with ROSAT. [Washington, DC: National Aeronautics and Space Administration, 1995.

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Voigt, H. H., ed. Stars and Star Clusters. Berlin/Heidelberg: Springer-Verlag, 1996. http://dx.doi.org/10.1007/b46101.

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Archinal, Brent A. Star clusters. Richmond, VA: Willmann-Bell, 2003.

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Cardona III, Charles A. Star Clusters. New York, NY: Springer New York, 2010. http://dx.doi.org/10.1007/978-1-4419-7040-4.

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Labhardt, Lukas, and Bruno Binggeli, eds. Star Clusters. Berlin/Heidelberg: Springer-Verlag, 2001. http://dx.doi.org/10.1007/3-540-31634-5.

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Space Telescope Science Institute (U. Massive Disk Formation Resulting From the Collision of A Main Sequence Star with A White Dwarf in A Globular Cluster Core. S.l: s.n, 1987.

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Hotka, Michael A. Globular Clusters Observing Club: A guide to observing globular clusters, objects selected by Leroy W.L. Guatney, an avid globular cluster observer. Kansas City, MO: Astronomical League, 2004.

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Goodman, Jeremy, and Piet Hut, eds. Dynamics of Star Clusters. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5335-2.

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Mirzoyan, L. V., B. R. Pettersen, and M. K. Tsvetkov, eds. Flare Stars in Star Clusters, Associations and the Solar Vicinity. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0607-5.

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1963-, Zepf Stephen E., ed. Globular cluster systems. Cambridge, U.K: Cambridge University Press, 1998.

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Book chapters on the topic "Star cluster"

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Benacquista, Matthew. "Star Cluster Dynamics." In An Introduction to the Evolution of Single and Binary Stars, 197–211. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4419-9991-7_14.

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Heggie, D. C. "Star Cluster Simulations." In Astrophysics and Space Science Library, 59–68. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0864-8_7.

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Bica, E. "Star and Star Cluster Spectral Libraries." In The Stellar Populations of Galaxies, 215–24. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2434-8_29.

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Fritze-v. Alvensleben, Uta. "Star Formation Efficiencies and Star Cluster Formation." In Starbursts, 209–14. Dordrecht: Springer Netherlands, 2005. http://dx.doi.org/10.1007/1-4020-3539-x_36.

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de Grijs, Richard. "Star Cluster Evolution: From Young Massive Star Clusters to Old Globulars." In Globular Clusters - Guides to Galaxies, 353–56. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-76961-3_81.

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Stevenson, David. "Globular Cluster Formation." In The Complex Lives of Star Clusters, 101–35. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-14234-0_4.

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Wan, Peng-Jun. "Multi-Star Cluster Interconnection Networks." In Network Theory and Applications, 187–201. Boston, MA: Springer US, 1999. http://dx.doi.org/10.1007/978-1-4615-5317-5_6.

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Andrews, D. F., and A. M. Herzberg. "Motions of Stars in a Star Cluster, M92." In Springer Series in Statistics, 139–46. New York, NY: Springer New York, 1985. http://dx.doi.org/10.1007/978-1-4612-5098-2_23.

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Hennebelle, Patrick. "Numerical Simulations of Cluster Formation." In The Birth of Star Clusters, 39–67. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-22801-3_2.

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Giannone, G., and D. Molteni. "The Role of Hard Binaries in Cluster Evolution." In Dynamics of Star Clusters, 321. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5335-2_36.

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Conference papers on the topic "Star cluster"

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Nikolov, Grigor, and Haralambi Markov. "Characterising LMC Star cluster NGC 2004." In 10th Jubilee International Conference of the Balkan Physical Union. Author(s), 2019. http://dx.doi.org/10.1063/1.5091219.

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RODRÍGUEZ-GONZÁLEZ, A., S. SILICH, and G. TENORIO-TAGLE. "OBSERVATIONAL MANIFESTATIONS FROM STAR CLUSTER WINDS." In Proceedings of the Guillermo Haro Conference 2003. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812702432_0064.

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Sizova, M. D., E. S. Postnikova, A. P. Demidov, N. V. Chupina, and S. V. Vereshchagin. "HYADES STAR CLUSTER AND A NEW COMETS." In 48-th International student's conferences "Physics of Space". Ural University Press, 2020. http://dx.doi.org/10.15826/b978-5-7996-2935-9.74.

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Wu, Jiapeng, and Yuncai Hao. "Research on Star Point Cluster Location Method." In 2022 2nd International Conference on Consumer Electronics and Computer Engineering (ICCECE). IEEE, 2022. http://dx.doi.org/10.1109/iccece54139.2022.9712767.

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Donahue, Megan, Sebastian Heinz, and Eric Wilcots. "Signatures of Star Formation in Brightest Cluster Galaxies." In THE MONSTER’S FIERY BREATH: FEEDBACK IN GALAXIES, GROUPS, AND CLUSTERS. AIP, 2009. http://dx.doi.org/10.1063/1.3293027.

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Fuller, Gary, Jan Forbrich, Jill Rathborne, Steven Longmore, and Sergio Molinari. "Star and Stellar Cluster Formation: ALMA-SKA Synergies." In Advancing Astrophysics with the Square Kilometre Array. Trieste, Italy: Sissa Medialab, 2015. http://dx.doi.org/10.22323/1.215.0152.

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Davis, John D., Suzanne Rivoire, and Moises Goldszmidt. "Star-Cap: Cluster Power Management Using Software-Only Models." In 2014 43nd International Conference on Parallel Processing Workshops (ICCPW). IEEE, 2014. http://dx.doi.org/10.1109/icppw.2014.27.

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BOZZA, V., and L. MANCINI. "GRAVITATIONAL LENSING OF S-STAR CLUSTER BY Sgr A." In Proceedings of the MG12 Meeting on General Relativity. WORLD SCIENTIFIC, 2012. http://dx.doi.org/10.1142/9789814374552_0435.

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Bortolas, Elisa, Michela Mapelli, and Mario Spera. "Star Cluster Disruption by a Supermassive Black Hole Binary." In Gravitational-waves Science&Technology Symposium. Trieste, Italy: Sissa Medialab, 2018. http://dx.doi.org/10.22323/1.325.0030.

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O’Dea, Christopher P., Alice Quillen, Jaehong Park, Nicholas Zufelt, Stefi A. Baum, George Privon, Jacob Noel-Storr, et al. "Spitzer Observations of Star Formation in Brightest Cluster Galaxies." In THE MONSTER’S FIERY BREATH: FEEDBACK IN GALAXIES, GROUPS, AND CLUSTERS. AIP, 2009. http://dx.doi.org/10.1063/1.3293029.

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Reports on the topic "Star cluster"

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Monteiro, Joana, Beatriz Kury, and Angela Da Rocha. The Role of Flagship Firms, External Actors and Support Institutions in the Emergence of Successful Export Activities in Brazil: Two Industrial Cluster Studies. Inter-American Development Bank, September 2009. http://dx.doi.org/10.18235/0011331.

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This paper examines the process by which firms in a cluster start to export based on systemic interactions and the process of diffusion of exporting as a business strategy within the cluster. Two Brazilian manufacturing industries are studied, and within each one a geographic cluster was identified as the origin of dynamic export growth. Players in each industrial cluster, as well as other significant players, were interviewed or identified using secondary sources, and extensive secondary data research was undertaken to study clusters' historical development. Detailed analysis and a comparison of the two experiences made it possible to draw some general conclusions concerning the similarities and differences between the two clusters in terms of the adoption and diffusion of exporting.
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Mason, Brian, William I. Hartkopf, Douglas R. Gies, Todd J. Henry, and Andrei A. Tokovinin. Speckle Interferometry of Massive and Cluster Stars. Fort Belvoir, VA: Defense Technical Information Center, September 2005. http://dx.doi.org/10.21236/ada480126.

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Kandrup, H. E., and P. J. Morrison. Hamiltonian structure of the Vlasov-Einstein system and the problem of stability for spherical relativistic star clusters. Office of Scientific and Technical Information (OSTI), November 1992. http://dx.doi.org/10.2172/10120708.

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Kandrup, H. E., and P. J. Morrison. Hamiltonian structure of the Vlasov-Einstein system and the problem of stability for spherical relativistic star clusters. Office of Scientific and Technical Information (OSTI), November 1992. http://dx.doi.org/10.2172/6789042.

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Press, W. H. (Astrophysics of binary stars, Seyfert galaxies, quasars, and globular clusters. Final technical report. Office of Scientific and Technical Information (OSTI), March 1985. http://dx.doi.org/10.2172/6429223.

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Meylan, G., D. Minniti, C. Pryor, C. G. Tinney, E. S. Phinney, and B. Sams. Proper motion with HST: Searching for high-velocity stars in the core of the globular cluster 47 Tucanae. Office of Scientific and Technical Information (OSTI), February 1996. http://dx.doi.org/10.2172/211576.

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Gerilla-Teknomo, Gloria P., and Jiawen Yang. Creating a Successful New City Development Within a City Cluster: Global Knowledge and Insights for Xiong’an in the People’s Republic of China. Asian Development Bank, March 2022. http://dx.doi.org/10.22617/wps220111-2.

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The presence of anchor institutions and transport infrastructure, strong national and local government policies, and business models with private sector participation can jump-start and sustain new city development. This paper has studied 16 major new city developments in the world to determine the factors that contributed to their success or failure. These factors were analyzed to synthesize useful knowledge and draw insights that the Xiong’an New Area in the People’s Republic of China and other new city developments in the world can learn from to better achieve their growth objectives.
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Menuhin, Jonathan. Innovation Ecosystem Management Methodology. Edited by Marcello Basani, Alejandro Minatta, and Cecilia Maroñas. Inter-American Development Bank, March 2024. http://dx.doi.org/10.18235/0012851.

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The main challenges innovation faces in the water, sanitation, and solid waste sector in Latin America and the Caribbean can be split into three categories: governance efforts; sector innovation ecosystem (research, development, and innovation), and water, sanitation, and solid waste utilities. In this line, it is key to acquire knowledge of international experiences to enrich the analysis and thematic discussion on the issue. The III (III) is an NGO that was established in 2011 to promote the development and implementation of innovation addressing global challenges such as transportation, climate change, health, agriculture, aquaculture, and desertification. To this end, The III established innovation ecosystems that connect relevant players with the fields they wish to promote, and created innovation opportunities, always acting objectively and impartially. Over the years, as the III gained experience, it formed a methodology that can be adjusted to and implemented in other sectors and fields to enhance their potential and address existing obstructions. Such methodology can be adopted by NGOs, countries, and regions according to the barriers their ecosystem experiences. Hence, a strategy that one ecosystem chooses may be different from the strategy that suits another. Yet, while the innovation clusters and ecosystems may vary, a common, organizing operational outline can be found in all. The methodology includes tools that were designed to match the development of innovation ecosystems facing new challenges and opportunities. This document opens with a presentation of the positive potential of forming and operating innovation ecosystems and the global trends that make them even more important (section I). The five fields of operation that promote innovation ecosystems are thus presented, each followed by practical examples of relevant tools: (1) market education; (2) social capital creation; (3) access to knowledge; (4) open innovation facilitation; and (5) internationalization in section, alongside practical tools to develop each layer, and the motivation for choosing each, which can assist in selecting from the extensive toolbox (Section II). Finally, some practical tips to start with the right foot are described (Section III).
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