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Relevant bibliographies by topics / Galaxy clusters/dynamics study

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Academic literature on the topic 'Galaxy clusters/dynamics study'

Author: Grafiati

Published: 4 June 2021

Last updated: 2 February 2022

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Journal articles on the topic "Galaxy clusters/dynamics study"

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Benavides, José A., Laura V. Sales, and Mario G. Abadi. "Accretion of galaxy groups into galaxy clusters." Monthly Notices of the Royal Astronomical Society 498, no. 3 (September 2, 2020): 3852–62. http://dx.doi.org/10.1093/mnras/staa2636.

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ABSTRACT We study the role of group infall in the assembly and dynamics of galaxy clusters in ΛCDM. We select 10 clusters with virial mass M200 ∼ 1014 $\rm M_\odot$ from the cosmological hydrodynamical simulation Illustris and follow their galaxies with stellar mass M⋆ ≥ 1.5 × 108 $\rm M_\odot$. A median of ${\sim}38{{\ \rm per\ cent}}$ of surviving galaxies at z = 0 is accreted as part of groups and did not infall directly from the field, albeit with significant cluster-to-cluster scatter. The evolution of these galaxy associations is quick, with observational signatures of their common origin eroding rapidly in 1–3 Gyr after infall. Substructure plays a dominant role in fostering the conditions for galaxy mergers to happen, even within the cluster environment. Integrated over time, we identify (per cluster) an average of 17 ± 9 mergers that occur in infalling galaxy associations, of which 7 ± 3 occur well within the virial radius of their cluster hosts. The number of mergers shows large dispersion from cluster to cluster, with our most massive system having 42 mergers above our mass cut-off. These mergers, which are typically gas rich for dwarfs and a combination of gas rich and gas poor for M⋆ ∼ 1011 $\rm M_\odot$, may contribute significantly within ΛCDM to the formation of specific morphologies, such as lenticulars (S0) and blue compact dwarfs in groups and clusters.

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Valenti, E., L. Origlia, and R. M. Rich. "Globular clusters in the near–infrared." Proceedings of the International Astronomical Union 5, H15 (November 2009): 555–56. http://dx.doi.org/10.1017/s1743921310010719.

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The study of Globular Cluster (GC) stellar populations (SPs) addresses fundamental astrophysical questions ranging from stellar structure, evolution and dynamics, to Galaxy formation. Indeed, they represent: i) fossils from the remote and violent epoch of Galaxy formation, ii) test particles for studying Galaxy dynamics and stellar dynamical model, and iii) fiducial templates for studying integrated light from distant stellar systems. In particular, high resolution spectroscopy of GC SPs provides abundance patterns which are crucial for understanding the formation and chemical enrichment time–scale of the host galaxy. Here the major results on Galactic GCs based on high-resolution near-infrared (near–IR) spectroscopy are briefly reviewed. Optical and IR spectroscopy are complementary tools to investigate SPs in different environments, the latter being more suitable in the case of moderately–high extinction regions (AV≥2) and high metallicity.

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Savini, F., A. Bonafede, M. Brüggen, D. Rafferty, T. Shimwell, A. Botteon, G. Brunetti, et al. "A LOFAR study of non-merging massive galaxy clusters." Astronomy & Astrophysics 622 (February 2019): A24. http://dx.doi.org/10.1051/0004-6361/201833882.

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Centrally located diffuse radio emission has been observed in both merging and non-merging galaxy clusters. Depending on their morphology and size, we distinguish between giant radio haloes, which occur predominantly in merging clusters, and mini haloes, which are found in non-merging, cool-core clusters. In recent years, cluster-scale radio emission has also been observed in clusters with no sign of major mergers, showing that our knowledge of the mechanisms that lead to particle acceleration in the intra-cluster medium (ICM) is still incomplete. Low-frequency sensitive observations are required to assess whether the emission discovered in these few cases is common in galaxy clusters or not. With this aim, we carried out a campaign of observations with the LOw Frequency ARay (LOFAR) in the frequency range 120–168 MHz of nine massive clusters selected from the Planck SZ catalogue, which had no sign of major mergers. In this paper, we discuss the results of the observations that have led to the largest cluster sample studied within the LOFAR Two-metre Sky Survey, and we present Chandra X-ray data used to investigate the dynamical state of the clusters, verifying that the clusters are currently not undergoing major mergers, and to search for traces of minor or off-axis mergers. We discover large-scale steep-spectrum emission around mini haloes in the cool-core clusters PSZ1G139.61+24 and RXJ1720.1+2638, which is not observed around the mini halo in the non-cool-core cluster A1413. We also discover a new 570 kpc-halo in the non-cool-core cluster RXCJ0142.0+2131. We derived new upper limits to the radio power for clusters in which no diffuse radio emission was found, and we discuss the implication of our results to constrain the cosmic-ray energy budget in the ICM. We conclude that radio emission in non-merging massive clusters is not common at the sensitivity level reached by our observations and that no clear connection with the cluster dynamical state is observed. Our results might indicate that the sloshing of a dense cool core could trigger particle acceleration on larger scales and generate steep-spectrum radio emission.

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John, Reju Sam, Surajit Paul, Luigi Iapichino, Karl Mannheim, and Harish Kumar. "Manufacturing cosmic rays in the evolving dynamical states of galaxy clusters." Monthly Notices of the Royal Astronomical Society 488, no. 1 (July 1, 2019): 1301–19. http://dx.doi.org/10.1093/mnras/stz1785.

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ABSTRACT Galaxy clusters are known to be reservoirs of cosmic rays (CRs), as inferred from theoretical calculations or detection of CR-derived observables. CR acceleration in clusters is mostly attributed to the dynamical activity that produces shocks. Shocks in clusters emerge out of merger or accretion, but which one is more effective in producing CRs? at which dynamical phase? and why? To this aim, we study the production or injection of CRs through shocks and its evolution in the galaxy clusters using cosmological simulations with the enzo code. Particle acceleration model considered here is primarily the Diffusive Shock Acceleration (DSA) of thermal particles, but we also report a tentative study with pre-existing CRs. Defining appropriate dynamical states using the concept of virialization, we studied a sample of merging and non-merging clusters. We report that the merger shocks (with Mach number $\mathcal {M}\sim 2-5$) are the most effective CR producers, while high-Mach peripheral shocks (i.e. $\mathcal {M}\gt 5$) are mainly responsible for the brightest phase of CR injection in clusters. Clusters once merged, permanently deviate from CR and X-ray mass scaling of non-merging systems, enabling us to use it as a tool to determine the state of merger. Through a temporal and spatial evolution study, we found a strong correlation between cluster merger dynamics and CR injection. We observed that the brightest phase of X-ray and CR injection from clusters occurs, respectively, at about 1.0 and 1.5 Gyr after every mergers, and CR injection peaks near to the cluster virial radius (i.e r200). Delayed CR injection peaks found in this study deserve further investigation for possible impact on the evolution of CR-derived observables from galaxy clusters.

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Roberts, Ian D., and Laura C. Parker. "‘Observing’ unrelaxed clusters in dark matter simulations." Monthly Notices of the Royal Astronomical Society 490, no. 1 (September 25, 2019): 773–83. http://dx.doi.org/10.1093/mnras/stz2666.

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ABSTRACT We present a detailed study of relaxed and unrelaxed galaxy clusters in a large dark matter only simulation. Recent work has demonstrated clear differences between the galaxy populations in clusters that have Gaussian velocity distributions (relaxed) compared to those that do not (unrelaxed). To directly compare with observations, we identify unrelaxed clusters in the simulations using one-dimensional velocity distributions. We show that non-Gaussian clusters have had recent major mergers and enhanced rates of galaxy infall relative to systems with Gaussian velocity profiles. Furthermore, we find that the fraction of non-Gaussian clusters increases strongly with cluster mass and modestly with redshift. For comparison, we also make use of three-dimensional information available in the simulations to explore the impact of projection on observational measurements. Differences between Gaussian and non-Gaussian clusters are much stronger when three-dimensional information is considered, which demonstrates that the strength of oberserved trends with cluster dynamics are diluted because observed velocity information is limited to one line-of-sight.

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Cuciti, V., R. Cassano, G. Brunetti, D. Dallacasa, F. de Gasperin, S. Ettori, S. Giacintucci, et al. "Radio halos in a mass-selected sample of 75 galaxy clusters." Astronomy & Astrophysics 647 (March 2021): A51. http://dx.doi.org/10.1051/0004-6361/202039208.

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Context. Many galaxy clusters host megaparsec-scale diffuse radio sources called radio halos. Their origin is tightly connected to the processes that lead to the formation of clusters themselves. In order to reveal this connection, statistical studies of the radio properties of clusters combined with their thermal properties are necessary. For this purpose, we selected a sample of galaxy clusters with M500 ≥ 6 × 1014 M⊙ and z = 0.08 − 0.33 from the Planck Sunyaev–Zel’dovich catalogue. In Paper I, we presented the radio and X-ray data analysis that we carried out on the clusters of this sample. Aims. In this paper we exploit the wealth of data presented in Paper I to study the radio properties of the sample, in connection to the mass and dynamical state of clusters. Methods. We used the dynamical information derived from the X-ray data to assess the role of mergers in the origin of radio halos. We studied the distribution of clusters in the radio power–mass diagram, the scaling between the radio luminosity of radio halos and the mass of the host clusters, and the role of dynamics in the radio luminosity and emissivity of radio halos. We measured the occurrence of radio halos as a function of the cluster mass and we compared it with the expectations of models developed in the framework of turbulent acceleration. Results. We find that more than the 90% of radio halos are in merging clusters and that their radio power correlates with the mass of the host clusters. The correlation shows a large dispersion. Interestingly, we show that cluster dynamics contributes significantly to this dispersion, with more disturbed clusters being more radio luminous. Clusters without radio halos are generally relaxed, and the upper limits to their diffuse emission lie below the correlation. Moreover, we show that the radio emissivity of clusters exhibits an apparent bimodality, with the emissivity of radio halos being at least ∼5 times larger than the non-emission associated with more relaxed clusters. We find that the fraction of radio halos drops from ∼70% in high-mass clusters to ∼35% in the lower mass systems in the sample and we show that this result is in good agreement with the expectations from turbulent re-acceleration models.

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Botteon, A., R. Cassano, D. Eckert, G. Brunetti, D. Dallacasa, T. W. Shimwell, R. J. van Weeren, et al. "Particle acceleration in a nearby galaxy cluster pair: the role of cluster dynamics." Astronomy & Astrophysics 630 (September 24, 2019): A77. http://dx.doi.org/10.1051/0004-6361/201936022.

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Context. Diffuse radio emission associated with the intracluster medium (ICM) is observed in a number of merging galaxy clusters. It is currently believed that a fraction of the kinetic energy in mergers is channeled into nonthermal components, such as turbulence, cosmic rays, and magnetic fields, which may lead to the formation of giant synchrotron sources in the ICM. Aims. Studying merging galaxy clusters in different evolutionary phases is fundamental for understanding the origin of radio emission in the ICM. Methods. We observed the nearby galaxy cluster pair RXC J1825.3+3026 (z ∼ 0.065) and CIZA J1824.1+3029 (z ∼ 0.071) at 120 − 168 MHz with the LOw Frequency ARray (LOFAR) and made use of a deep (240 ks) XMM-Newton dataset to study the nonthermal and thermal properties of the system. RXC J1825.3+3026 is in a complex dynamical state, with a primary ongoing merger in the E-W direction and a secondary later stage merger with a group of galaxies in the SW, while CIZA J1824.1+3029 is dynamically relaxed. These two clusters are in a pre-merger phase. Results. We report the discovery of a Mpc-scale radio halo with a low surface brightness extension in RXC J1825.3+3026 that follows the X-ray emission from the cluster center to the remnant of a galaxy group in the SW. This is among the least massive systems and the faintest giant radio halo known to date. In contrast to this, no diffuse radio emission is observed in CIZA J1824.1+3029, nor in the region between the pre-merger cluster pair. The power spectra of the X-ray surface brightness fluctuations of RXC J1825.3+3026 and CIZA J1824.1+3029 are in agreement with the findings for clusters exhibiting a radio halo and clusters where no radio emission has been detected, respectively. Conclusions. We provide quantitative support to the idea that cluster mergers play a crucial role in the generation of nonthermal components in the ICM.

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Einasto, Maret, Boris Deshev, Heidi Lietzen, Rain Kipper, Elmo Tempel, Changbom Park, Mirt Gramann, Pekka Heinämäki, Enn Saar, and Jaan Einasto. "Infalling groups and galaxy transformations in the cluster A2142." Astronomy & Astrophysics 610 (February 2018): A82. http://dx.doi.org/10.1051/0004-6361/201731600.

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Context. Superclusters of galaxies provide dynamical environments for the study of the formation and evolution of structures in the cosmic web from galaxies, to the richest galaxy clusters, and superclusters themselves. Aims. We study galaxy populations and search for possible merging substructures in the rich galaxy cluster A2142 in the collapsing core of the supercluster SCl A2142, which may give rise to radio and X-ray structures in the cluster, and affect galaxy properties of this cluster. Methods. We used normal mixture modelling to select substructure of the cluster A2142. We compared alignments of the cluster, its brightest galaxies (hereafter BCGs), subclusters, and supercluster axes. The projected phase space (PPS) diagram and clustercentric distributions are used to analyse the dynamics of the cluster and study the distribution of various galaxy populations in the cluster and subclusters. Results. We find several infalling galaxy groups and subclusters. The cluster, supercluster, BCGs, and one infalling subcluster are all aligned. Their orientation is correlated with the alignment of the radio and X-ray haloes of the cluster. Galaxy populations in the main cluster and in the outskirts subclusters are different. Galaxies in the centre of the main cluster at the clustercentric distances 0.5 h−1 Mpc (Dc∕Rvir < 0.5, Rvir = 0.9 h−1 Mpc) have older stellar populations (with the median age of 10−11 Gyr) than galaxies at larger clustercentric distances. Star-forming and recently quenched galaxies are located mostly at the clustercentric distances Dc ≈ 1.8 h−1 Mpc, where subclusters fall into the cluster and the properties of galaxies change rapidly. In this region the median age of stellar populations of galaxies is about 2 Gyr. Galaxies in A2142 on average have higher stellar masses, lower star formation rates, and redder colours than galaxies in rich groups. The total mass in infalling groups and subclusters is M ≈ 6 × 1014 h−1 M⊙, that is approximately half of the mass of the cluster. This mass is sufficient for the mass growth of the cluster from redshift z = 0.5 (half-mass epoch) to the present. Conclusions. Our analysis suggests that the cluster A2142 has formed as a result of past and present mergers and infallen groups, predominantly along the supercluster axis. Mergers cause complex radio and X-ray structure of the cluster and affect the properties of galaxies in the cluster, especially at the boundaries of the cluster in the infall region. Explaining the differences between galaxy populations, mass, and richness of A2142, and other groups and clusters may lead to better insight about the formation and evolution of rich galaxy clusters.

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Stasyszyn, F. A., and M. de los Rios. "Faraday rotation measure dependence on galaxy cluster dynamics." Monthly Notices of the Royal Astronomical Society 487, no. 4 (June 28, 2019): 4768–74. http://dx.doi.org/10.1093/mnras/stz1450.

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ABSTRACT We study the magnetic fields in galaxy clusters through Faraday rotation measurements crossing systems in different dynamical states. We confirm that magnetic fields are present in those systems and analyse the difference between relaxed and unrelaxed samples with respect to the dispersion between their inherent Faraday rotation measurements (RM). We found an increase of this RM dispersion and a higher RM overlapping frequency for unrelaxed clusters. This fact suggests that a large-scale physical process is involved in the nature of unrelaxed systems and possible depolarization effects are present in the relaxed ones. We show that dynamically unrelaxed systems can enhance magnetic fields to large coherence lengths. In contrast, the results for relaxed systems suggests that a small-scale dynamo can be a dominant mechanism for sustaining magnetic fields, leading to intrinsic depolarization.

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Peña, J. H., and R. Peniche. "Photometry of early type stars in open clusters (NGC 1444, NGC 1662, NGC 2129, NGC 2169 and NGC 7209)." Symposium - International Astronomical Union 162 (1994): 303–4. http://dx.doi.org/10.1017/s0074180900215143.

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This is part of a series which has the purpose of examining the nature of the stars belonging to open clusters. The aim of this series is, among others things, to study short period pulsating stars, mainly of the Delta Scuti type, by first establishing the membership of each star to the cluster, to determine the abundance of the Be and Ap phenomena and blue stragglers in open clusters for clusters of different ages and metalicities and, eventually, to study the chemical enrichment of the galaxy when age, dynamics and metalicity are known for a fair number of clusters.

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Dissertations / Theses on the topic "Galaxy clusters/dynamics study"

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Millington, S. J. C. "Clusters of galaxies." Thesis, University of Oxford, 1987. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.382461.

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Drake, Nick. "Wakes and dynamics of galaxy clusters." Thesis, University of Southampton, 2000. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.326792.

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Parekh, Viral. "Morphological classification and dynamics of X-ray galaxy clusters." Doctoral thesis, University of Cape Town, 2014. http://hdl.handle.net/11427/9539.

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Braglia, Filiberto Giorgio. "Study of optical properties and galaxy populations of galaxy clusters." Diss., kostenfrei, 2008. http://edoc.ub.uni-muenchen.de/9179/.

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Nastasi, Alessandro. "Multiwavelength Study of high redshift galaxy clusters." Diss., lmu, 2012. http://nbn-resolving.de/urn:nbn:de:bvb:19-152323.

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Hodson, Alistair. "A non-Newtonian perspective of gravity : testing modified gravity theories in galaxies and galaxy clusters." Thesis, University of St Andrews, 2017. http://hdl.handle.net/10023/12016.

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This thesis attempts to test several frameworks of non-Newtonian gravity in the context of galaxies and galaxy clusters. The theory most extensively discussed was that of Modiﬁed Newtonian Dynamics (MOND) with Galileon gravity, Emergent Gravity (EG) and Modiﬁed Gravity (MOG) mentioned to a lesser extent. Speciﬁcally, the main focus of this thesis was to determine whether MOND and MOND-like theories were compatible with galaxy cluster data, without the need to include cold dark matter. To do this, the paradigms of Extended MOND (EMOND), Generalised MOND (GMOND) and superﬂuid dark matter were investigated. The theories were outlined and applied to galaxy cluster data. The main ﬁndings of this were that EMOND and GMOND had some success with explaining galaxy cluster mass proﬁles, without requiring an additional dark matter component. The superﬂuid paradigm also enjoyed some success in galaxy clusters, which was expected as it behaves in a similar manner to the standard cold dark matter paradigm in cluster environments. However, the superﬂuid paradigm may have issues in the very centre of galaxy clusters due to the theory predicting constant density cores, whereas the cold dark matter paradigm predicts density cores which are cuspier. The EMOND paradigm was also tested against ultra-diffuse galaxy (UDGs) data as they appear in cluster environments, where EMOND becomes important. It was found that EMOND can reproduce the inferred mass of the UDGs, assuming they lie on the fundamental manifold (FM). The validity of the assumptions used to model the UDGs are discussed in the text. A two-body problem was also conducted in the Galileon gravity framework. The amount of additional gravitational force, compared to Newtonian was determined for a small galaxy at the edge of a galaxy cluster.

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Moran, Sean M. Djorgovski S. G. Ellis Richard S. "Understanding the physical processes driving galaxy evolution in clusters : a case study of two z~0.5 galaxy clusters /." Diss., Pasadena, Calif. : California Institute of Technology, 2008. http://resolver.caltech.edu/CaltechETD:etd-08212007-151300.

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Winkworth, Carolyn Louise. "An Observational Study of High Redshift Galaxy Clusters." Thesis, University of Bristol, 2009. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.520307.

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Renaud, Florent. "Dynamics of the Tidal Fields and Formation of Star Clusters in Galaxy Mergers." Phd thesis, Université de Strasbourg, 2010. http://tel.archives-ouvertes.fr/tel-00508301.

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Dans les galaxies en interaction, de colossales forces de marée perturbent la morphologie des progéniteurs pour engendrer les longs bras d'étoiles, gaz et poussières que l'on observe parfois. En plus de leur effet destructeur, les forces de marée peuvent, dans certain cas, se placer dans une configuration protectrice appelée mode compressif. De tels modes protègent alors la matière en leur sein, en augmentant son énergie de liaison. Cette thèse se concentre sur l'étude de ce régime peu connu en quantifiant ses propriétés grâce à des outils numériques et analytiques appliqués à un spectaculaire système de galaxies en fusion, communément appelé les Antennes. Des simulations N-corps de cette paire de galaxies montrent la présence de modes compressifs dans les régions où les observations révèlent un sursaut de formation stellaire. De plus, les temps et énergies caractéristiques de ces modes correspondent à ceux de la formation de sous-structures autogravitantes telles que des amas stellaires et des naines de marée. Des comparaisons avec les taux de formation stellaire dérivés de simulations hydrodynamiques confirment la corrélation entre les positions des modes compressifs et les sites où la formation des étoiles est certainement amplifiée. Mis bout-à-bout, ces résultats suggèrent que les modes compressifs des champs de marée jouent un role important dans la formation et l'évolution des jeunes amas, au moins d'un point de vue statistique, sur une échelle de temps de l'ordre de dix millions d'années. Des résultats préliminaires de simulations d'associations stellaires soulignent l'importance de plonger les amas dans leur environnement galactique en évolution, pour tenir compte précisément de leur morphologie et évolution interne. Ces conclusions ont été étendues à de nombreuses configurations d'interaction et restent robustes aux variations des principaux paramètres caractérisant les paires de galaxies. Nous notons cependant une nette anti-corrélation entre l'importance du mode compressif et la distance entre ces galaxies. De nouvelles études incluant les aspects hydrodynamiques sont maintenant en cours et aideront à préciser le rôle exact du mode compressif dans la formation et la survie des amas d'étoiles. Les premières comparaisons avec de telles simulations suggèrent que les modes compressifs agissent en tant que catalyseurs ou amorces de la formation stellaire.

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Hall, Emily Anne. "Clusters and cosmic onions : a description of galaxy dynamics in the quasi-linear regime." Thesis, University College London (University of London), 2018. http://discovery.ucl.ac.uk/10057210/.

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This thesis investigates the dynamics of galaxies around clusters in the quasi-linear regime, with the ultimate aim of providing cluster mass constraints which can be combined with weak lensing measurements in order to perform tests of General Relativity. Dark matter simulations are populated with galaxies using a halo occupation distribution, and used to develop and test models which describe di↵erent aspects of galaxy dynamics around clusters. A heuristic analytical model is presented describing the infall profile of galaxies onto a cluster of given mass, which is shown to fit the simulations remarkably well on quasilinear scales. The velocity dispersion of galaxies in the simulations is also examined, and a model developed which describes how this e↵ect varies as a function of position relative to the cluster centre. These models of galaxy infall and velocity dispersion are combined to provide predictions of the cluster-galaxy redshift space correlation function, or cosmic onion, which show a relatively good agreement with the simulations. The cosmic onion model is used to obtain cluster mass constraints from redshift space distortions observed in the simulations, in order to demonstrate the robustness of this method. In this work the uncertainty on cluster mass was estimated with all other halo parameters fixed, and was found to be approximately 2% at the 2 confidence level for a halo mass of ⇠ 1013 Msolarh1. However in practice the accuracy of these constraints depends on how many free parameters are considered in the halo occupation distribution, as some are degenerate with the cluster mass. The techniques developed here can be applied to observational data from the upcoming generation of spectroscopic galaxy surveys, potentially improving constraints on the dynamic mass of clusters measured from redshift space distortions.

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Books on the topic "Galaxy clusters/dynamics study"

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David, Merritt. Galaxy Dynamics: A Rutgers Symposium. San Francisco, Calif: Astronomical Society of the Pacific, 1999.

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Hartog, Roland Henrik den. The dynamics of rich galaxy clusters: Proefschrift. Leiden: Sterrewacht, 1995.

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Blindert, Kris. Internal dynamics of galaxy clusters in the Red-Sequence Cluster Survey. 2006.

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1949-, Lagnevik Magnus, ed. The dynamics of innovation clusters: A study of the food industry. Northhampton, MA: Edward Elgar Pub., 2003.

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Lagnevik, Magnus, Ingegerd Sjoholm, Anders Lareke, and Jacob Ostberg. The Dynamics of Innovation Clusters: A Study of the Food Industry (New Horizons in the Economics of Innovation). Edward Elgar Publishing, 2003.

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Danilov, V. M. Non-stationarity of Open Star Clusters. Ural University Press, 2021. http://dx.doi.org/10.15826/b978-5-7996-3173-4.

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The monograph poses issues related to the study of the non-stationarity of open star clusters (OSCs), starting with an analysis of the properties of the trajectories of individual stars to the study of collective motion of stars. A discussion of the dynamics of correlations and wave processes in such clusters is presented. The mechanisms of the dynamic evolution of OSCs, the gravitational instability of OSC nuclei, the spectra of frequencies and wavenumbers for oscillations of numerical models of OSCs, astrophysical applications of the results of studies of the dynamics of OSCs are considered. We address the monograph to academic researchers (astronomers and physicists) who are interested in astrophysics, the dynamics of stellar systems, and PhD and senior students of relevant specialities.

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Baer, Tomas, and William L. Hase. Unimolecular Reaction Dynamics. Oxford University Press, 1996. http://dx.doi.org/10.1093/oso/9780195074949.001.0001.

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This book provides a penetrating and comprehensive description of energy selected reactions from a theoretical as well as experimental view. Three major aspects of unimolecular reactions involving the preparation of the reactants in selected energy states, the rate of dissociation of the activated molecule, and the partitioning of the excess energy among the final products, are fully discussed with the aid of 175 illustrations and over 1,000 references, most from the recent literature. Examples of both neutral and ionic reactions are presented. Many of the difficult topics are discussed at several levels of sophistication to allow access by novices as well as experts. Among the topics covered for the first time in monograph form is a discussion of highly excited vibrational/rotational states and intramolecular vibrational energy redistribution. Problems associated with the application of RRKM theory are discussed with the aid of experimental examples. Detailed comparisons are also made between different statistical models of unimolecular decomposition. Both quantum and classical models not based on statistical assumptions are described. Finally, a chapter devoted to the theory of product energy distribution includes the application of phase space theory to the dissociation of small and large clusters. The work will be welcomed as a valuable resource by practicing researchers and graduate students in physical chemistry, and those involved in the study of chemical reaction dynamics.

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Book chapters on the topic "Galaxy clusters/dynamics study"

1

Džanović, Dajana, R. M. Sharples, A. J. Benson, and C. S. Frenk. "Quantitative Study of Galaxy Morphology." In Galaxy Evolution in Groups and Clusters, 73–77. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0107-6_10.

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Godwin, P. J. "Core and Tidal Radii of the Carina Dwarf Spheroidal Galaxy from UK Schmidt Telescope Plates." In Dynamics of Star Clusters, 77–79. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5335-2_9.

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van Leeuwen, Floor. "A Proper Motion Study of the Pleiades Cluster." In Dynamics of Star Clusters, 477–80. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5335-2_55.

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Massobrio, Carlo, and Brahim Nacer. "Collisional dynamics of Ag19 on Pd(100): a molecular dynamics study." In Small Particles and Inorganic Clusters, 526–29. Berlin, Heidelberg: Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/978-3-642-60854-4_126.

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Wang, Q., M. P. Iñiguez, and J. A. Alonso. "Molecular dynamics study of A18B Lennard-Jones clusters." In Atomic and Nuclear Clusters, 294–96. Berlin, Heidelberg: Springer Berlin Heidelberg, 1995. http://dx.doi.org/10.1007/978-3-642-79696-8_76.

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Blaisten-Barojas, Estela, and D. Levesque. "A Molecular Dynamics Study of Silicon Clusters." In Physics and Chemistry of Small Clusters, 157–68. Boston, MA: Springer US, 1987. http://dx.doi.org/10.1007/978-1-4757-0357-3_25.

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Lugger, Phyllis M. "An Investigation of the Radial Dependence of the Galaxy Luminosity Function in Abell Clusters." In Structure and Dynamics of Elliptical Galaxies, 459–60. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3971-4_72.

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Mathieu, Robert D. "$$\lambda $$ λ Ori: A Case Study in Star Formation." In Dynamics of Young Star Clusters and Associations, 147–63. Berlin, Heidelberg: Springer Berlin Heidelberg, 2015. http://dx.doi.org/10.1007/978-3-662-47290-3_11.

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Richert, R., S. Y. Goldberg, B. Fainberg, and D. Huppert. "Ultrafast Solvation Dynamics by Degenerate Four Wave Mixing: A Theoretical and Experimental Study." In Reaction Dynamics in Clusters and Condensed Phases, 227–44. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0786-0_17.

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Zhao, Jijun. "The Coordination and Dynamic Analysis of Industrial Clusters: A Multi-agent Simulation Study." In Optimization and Dynamics with Their Applications, 105–25. Singapore: Springer Singapore, 2017. http://dx.doi.org/10.1007/978-981-10-4214-0_7.

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Conference papers on the topic "Galaxy clusters/dynamics study"

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Battistelli, Elia. "Sunyaev Zel’dovich study of filamentary structuresbetween galaxy clusters." In Multifrequency Behaviour of High Energy Cosmic Sources - XIII. Trieste, Italy: Sissa Medialab, 2020. http://dx.doi.org/10.22323/1.362.0008.

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LOBO, C., and M. SEROTE ROOS. "STUDY OF THREE GALAXY CLUSTERS AT INTERMEDIATE REDSHIFTS." In Proceedings of the 15th Portuguese National Meeting. WORLD SCIENTIFIC, 2006. http://dx.doi.org/10.1142/9789812773067_0013.

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Ferrari, C., Arwa Dabbech, Oleg Smirnov, Sphesihle Makhathini, Jonathan Simon Kenyon, Matteo Murgia, Federica Govoni, et al. "Non-thermal emission from galaxy clusters: feasibility study with SKA." In Advancing Astrophysics with the Square Kilometre Array. Trieste, Italy: Sissa Medialab, 2015. http://dx.doi.org/10.22323/1.215.0075.

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FAMAEY, B., G. W. ANGUS, G. GENTILE, H. Y. SHAN, and H. S. ZHAO. "THE WEDDING OF MODIFIED DYNAMICS AND NON-EXOTIC DARK MATTER IN GALAXY CLUSTERS." In Proceedings of the 6th International Heidelberg Conference. WORLD SCIENTIFIC, 2008. http://dx.doi.org/10.1142/9789812814357_0039.

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Giacintucci, S., J. M. Vrtilek, E. O’Sullivan, S. Raychaudhury, L. P. David, T. Venturi, R. Athreya, M. Gitti, Sebastian Heinz, and Eric Wilcots. "AGN Feedback in Galaxy Groups: A Joint GMRT∕X-ray Study." In THE MONSTER’S FIERY BREATH: FEEDBACK IN GALAXIES, GROUPS, AND CLUSTERS. AIP, 2009. http://dx.doi.org/10.1063/1.3293043.

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DING, FENG, KIM BOLTON, and ARNE ROSÉN. "MOLECULAR DYNAMICS STUDY OF IRON CLUSTER COALESCENCE AT SUB-MELTING POINT TEMPERATURES." In Clusters and Nano-Assemblies - Physical and Biological Systems. WORLD SCIENTIFIC, 2005. http://dx.doi.org/10.1142/9789812701879_0008.

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Victor Ribeiro de Jesus, João, and Rodrigo Lyra. "Um Estudo Sobre Identificação de Aglomerados de Galáxias." In Computer on the Beach. Itajaí: Universidade do Vale do Itajaí, 2020. http://dx.doi.org/10.14210/cotb.v11n1.p048-049.

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Galaxy clusters are fundamental blocks of our universe, like stars and galaxies. The study of galaxy clusters has shown complexity due to a large number of stars superimposed on these clusters, which emit light and block the clear optical band visualization of the phenomenon. In this paper, we present the implementation of an algorithm capable of classifying and remove the stars of spatial images. The purpose is to improve not only the existing studies around galaxy clusters but also to assist the developing in astronomic researches with available treated spatial images.

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Suzuki, Masaaki, Hiroshi Okuda, and Genki Yagawa. "Large-Scale Biomolecular Dynamics Using SMP Clusters." In 12th International Conference on Nuclear Engineering. ASMEDC, 2004. http://dx.doi.org/10.1115/icone12-49573.

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The authors have applied Message Passing Interface (MPI) / OpenMP hybrid parallel programming model to molecular dynamics (MD) method for simulating a protein structure on a symmetric multiprocessor (SMP) cluster architecture. In that architecture, it can be expected that the hybrid parallel programming model, which uses the message passing library such as MPI for inter-SMP node communication and the loop directives such as OpenMP for intra-SMP node parallelization, is the most effective one. In this study, the parallel performance of the hybrid style has been compared with that of conventional flat parallel programming style, which uses only MPI, both in case that the fast multipole method (FMM) is employed for computing long-distance interactions and that is not employed. The computer environments used here are Hitachi SR8000/MPP placed at the University of Tokyo. The results of calculation are as follows: Without using FMM, the parallel efficiency using 16 SMP nodes (128 PEs) is: - 90% with the hybrid style, - 75% with the flat-MPI style, for MD simulation with 33,402 atoms. With FMM, the parallel efficiency using 16 SMP nodes (128 PEs) is: - 60% with the hybrid style, - 48% with the flat-MPI style, for MD simulation with 117,649 atoms.

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Chen, Min. "Characteristics of Helium Diffusion Trajectory: A Molecular Dynamics Study." In 2013 21st International Conference on Nuclear Engineering. American Society of Mechanical Engineers, 2013. http://dx.doi.org/10.1115/icone21-16466.

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Molecular dynamics (MD) are employed to explore the features of Helium atom and He clusters diffusion in titanium at the temperatures between room temperature and 667k. The results demonstrate that the frequency for Helium atom jumping from site to site increases with the increasing temperature. Another important feature is that the diffusion of a He atom and a He trimer is a layered structure. The difference is that the trajectory of a He atom is between two Ti atom layers of (001) planes, and the trajectory of a He trimer is overlapped with the Ti atom layers of (001) plane. Meanwhile, it is observed that the layered structured diffusion becomes ambiguous for a He atom and a He trimer when the temperature is increased. The conclusion emphasizes different migration features for He clusters of various sizes.

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Desfrançois, C., and J. P. Schermann. "A collisional approach for the study of electron solvation in water and ammonia clusters and autodetachment of solvated molecular anions." In Ultrafast reaction dynamics and solvent effects. AIP, 1994. http://dx.doi.org/10.1063/1.45413.

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