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Journal articles on the topic 'Dynamical large-N'

Author: Grafiati

Published: 4 June 2021

Last updated: 6 February 2022

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1

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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Hotta, Tomohiro, Jun Nishimura, and Asato Tsuchiya. "Dynamical aspects of large-N reduced models." Nuclear Physics B 545, no. 1-3 (1999): 543–75. http://dx.doi.org/10.1016/s0550-3213(99)00056-5.

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Hotta, T., J. Nishimura, and A. Tsuchiya. "Dynamical properties of large N reduced model of Yang-Mills theory." Nuclear Physics B - Proceedings Supplements 73, no. 1-3 (1999): 810–12. http://dx.doi.org/10.1016/s0920-5632(99)85211-6.

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Dhar, Avinash, Gautam Mandal, and Spenta R. Wadia. "Leading large N modification of QCD2 on a cylinder by dynamical fermions." Nuclear Physics B 436, no. 3 (1995): 487–506. http://dx.doi.org/10.1016/0550-3213(94)00535-m.

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Wang, Long, Rainer Spurzem, Sverre Aarseth, et al. "Acceleration of hybrid MPI parallel NBODY6++ for large N-body globular cluster simulations." Proceedings of the International Astronomical Union 10, S312 (2014): 260–61. http://dx.doi.org/10.1017/s174392131500798x.

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AbstractPrevious research on globular clusters (GCs) dynamics is mostly based on semi-analytic, Fokker-Planck, Monte-Carlo methods and on direct N-body (NB) simulations. These works have great advantages but also limits since GCs are massive and compact and close encounters and binaries play very important roles in their dynamics. The former three methods make approximations and assumptions, while expensive computing time and number of stars limit the latter method. The current largest direct NB simulation has ~ 500k stars (Heggie 2014). Here, we accelerate the direct NB code NBODY6++ (which e

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Watanabe, K., Y. Kikuchi, K. Hiratsuka, and H. Yamaguchi. "A new approach for n-beam dynamical calculations." Acta Crystallographica Section A Foundations of Crystallography 46, no. 2 (1990): 94–98. http://dx.doi.org/10.1107/s0108767389010135.

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With the use of modulated plane waves, a new method for n-beam dynamical calculations has been established on the basis of a paper by Watanabe, Kikuchi, Hiratsuka & Yamaguchi [Phys. Status Solidi A (1988), 109, 119-126]. The computing time is reduced to about one-sixth of what it originally was and a large reduction of memory is achieved, n-beam dynamical calculations of aluminium, copper and gold at several accelerating voltages and orientations were carried out in a completely parallel manner by the present method, the multi-slice method and Bethe's eigen-value method [Fujiwara (1959). J

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Pieprzyk, Sławomir, Marcus N. Bannerman, Arkadiusz C. Brańka, Maciej Chudak, and David M. Heyes. "Thermodynamic and dynamical properties of the hard sphere system revisited by molecular dynamics simulation." Physical Chemistry Chemical Physics 21, no. 13 (2019): 6886–99. http://dx.doi.org/10.1039/c9cp00903e.

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Revised thermodynamic and dynamical properties of the hard sphere (HS) system are obtained from extensive molecular dynamics calculations carried out with large system sizes (number of particles, N) and long times.

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Hibbard, J. E., and J. E. Barnes. "The Dynamical Masses of Tidal Dwarf Galaxies." Symposium - International Astronomical Union 217 (2004): 510–17. http://dx.doi.org/10.1017/s0074180900198298.

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A variety of substructures have been identified within the tidal debris around interacting galaxies. These structures range in scale from Globular Clusters to the so-called “Tidal Dwarf Galaxies”. We review observations of such objects, with particular emphasis on what can be inferred from dynamical mass estimates. We then present the results of a dynamical analysis of structures which develop within the tidal tails of a large-N numerical simulation (N~1 million). We find that under the best conditions, “observations” of this system recover the true mass of the bound substructures to within a

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Jia, Duojie, Ruibin Wan, and Lianchun Yu. "A dynamical mass and confinement in nucleon model." International Journal of Modern Physics E 23, no. 06 (2014): 1460004. http://dx.doi.org/10.1142/s0218301314600040.

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A possible dynamical softening of the Chiral bag is studied in connection with the chiral quark model and the Nambu–Jona–Lasinio (NJL) model. It is demonstrated that the bag functions constructed by the pion degrees is able to confine quark through generation of the rising effective mass of valence quark due to the pion dressing and break chiral symmetry dynamically. The tendency of the bag functions toward the MIT bag is illustrated in the large-n limit for a solitonic configuration of the chiral field Un(r) for which U1(r) is the Skyrmion profile. The mass running with the length scale agree

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Wilkinson, Mark I., Gerard F. Gilmore, and Jarrod Hurley. "Dynamical Evolution of Rich Star Clusters in the LMC." Symposium - International Astronomical Union 207 (2002): 577–83. http://dx.doi.org/10.1017/s007418090022439x.

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We combine the results of a large HST study of rich LMC clusters with state of the art N-body simulations. We summarise recent highlights from our project: the estimation of age spreads in young LMC clusters, the measurement of the binary fraction of NGC1818, and the determination of deep cluster luminosity functions (LF). We also present preliminary results from an investigation of the core radius versus age relation evident among LMC clusters.

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SONG, DAE-YUP. "DYNAMICAL MASS GENERATION AND CRITICAL CURVATURE IN THE O(N) NONLINEAR SIGMA MODEL." Modern Physics Letters A 11, no. 19 (1996): 1569–78. http://dx.doi.org/10.1142/s0217732396001569.

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The large-N nonlinear O(N) sigma model with the curvature coupled term ξRn2 is examined on a spacetime of R1×S2 topology (three-dimensional static Einstein universe). Making use of the cutoff method, we find the renormalized effective potential which shows that, for ξ>1/8, there is a second-order phase transition. Above the critical curvature, the dynamical mass generation does not take place even in the strong-coupled regime. The phase structure of the model on S2 is also discussed.

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12

GLASNER, ELI. "The structure of tame minimal dynamical systems." Ergodic Theory and Dynamical Systems 27, no. 6 (2007): 1819–37. http://dx.doi.org/10.1017/s0143385707000296.

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AbstractA dynamical version of the Bourgain–Fremlin–Talagrand dichotomy shows that the enveloping semigroup of a dynamical system is either very large and contains a topological copy of $\beta \mathbb {N}$, or it is a ‘tame’ topological space whose topology is determined by the convergence of sequences. In the latter case, the dynamical system is said to be tame. We use the structure theory of minimal dynamical systems to show that, when the acting group is Abelian, a tame metric minimal dynamical system (i) is almost automorphic (i.e. it is an almost one-to-one extension of an equicontinuous

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BASS, R. W., and A. DEL POPOLO. "DYNAMICAL DERIVATION OF BODE'S LAW." International Journal of Modern Physics D 14, no. 01 (2005): 153–69. http://dx.doi.org/10.1142/s0218271805006195.

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In a planetary or satellite system, idealized as n small bodies in an initially coplanar with concentric orbits around a large central body obeying the Newtonian point-particle mechanics, resonant perturbations will cause a dynamical evolution of the orbital radii except for cases with highly specific mutual relationships. In particular, the most stable situation can be achieved only when each planetary orbit is roughly twice as far from the Sun as the preceding one. This has been empirically observed by Titius (1766) and Bode (1778). By reformulating the problem as a hierarchical sequence of

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Gardiner, L. T. "Review of N-Body Models of Tidal Interactions." Symposium - International Astronomical Union 190 (1999): 480–86. http://dx.doi.org/10.1017/s0074180900118662.

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Considerable progress has been made in the current decade with the help of N-body simulations towards a deeper understanding of the nature of the dynamical relationship between the Large and Small Magellanic Clouds and the Galaxy. The origin of such features as the Magellanic Stream, the inter-Cloud Bridge, the Wing and large extension in depth of the SMC has come to be interpreted in the context of the tidal interactions among the members of the LMC-SMC-Galaxy triple system. The inclusion of gas-dynamical effects and star formation in the latest models has added further refinements to this pi

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Yang, Shengqi, Xiaolong Du, Andrew J. Benson, Anthony R. Pullen, and Annika H. G. Peter. "A new calibration method of sub-halo orbital evolution for semi-analytic models." Monthly Notices of the Royal Astronomical Society 498, no. 3 (2020): 3902–13. http://dx.doi.org/10.1093/mnras/staa2496.

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ABSTRACT Understanding the non-linear dynamics of satellite haloes (a.k.a. ‘sub-haloes’) is important for predicting the abundance and distribution of dark matter sub-structures and satellite galaxies, and for distinguishing among microphysical dark matter models using observations. Typically, modelling these dynamics requires large N-body simulations with high resolution. Semi-analytic models can provide a more efficient way to describe the key physical processes such as dynamical friction, tidal mass loss, and tidal heating, with only a few free parameters. In this work, we present a fast Ma

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Gerber, Richard A., Dinshaw S. Balsara, and Susan A. Lamb. "Dynamical Experiments on Models of Colliding Disk Galaxies." International Astronomical Union Colloquium 124 (1990): 737–42. http://dx.doi.org/10.1017/s025292110000590x.

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Collisions between galaxies can induce large morphological changes in the participants and, in the case of colliding disk galaxies, bridges and tails are often formed. Observations of such systems indicate a wide variation in color (see Larson and Tinsley, 1978) and that some of the participants are experiencing enhanced rates of star formation, especially in their central regions (Bushouse 1986, 1987; Kennicutt et al., 1987, Bushouse, Lamb, and Werner, 1988). In this paper we describe progress we have made in understanding some of the dynamics of interacting galaxies using N-body stellar dyna

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Kiseleva, Ludmila, and Joanna Anosova. "Criteria of Dynamical Isolation of Binaries and Multiples." Symposium - International Astronomical Union 169 (1996): 531–32. http://dx.doi.org/10.1017/s0074180900230301.

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In order to obtain an objective criterion for dynamical isolation of binaries within systems of large multiplicity we study numerically the dynamical behavior and average parameters of stable hierarchical triple systems containing a close binary. Using the new criterion for hierarchical stability of triple systems with different mass ratios of components (Kiseleva, Eggleton, Anosova 1994; Kiseleva, Eggleton, Orlov 1994) the perturbing force from the outer body on the close inner binary is estimated. On this basis, the critical separations are obtained when both inner and outer orbits are pract

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Lorek, Sebastian, and Anders Johansen. "A close-encounter method for simulating the dynamics of planetesimals." Astronomy & Astrophysics 644 (November 24, 2020): A14. http://dx.doi.org/10.1051/0004-6361/202037540.

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The dynamics of planetesimals plays an important role in planet formation because their velocity distribution sets the growth rate to larger bodies. When planetesimals form in the gaseous environment of protoplanetary discs, their orbits are nearly circular and planar due to the effect of gas drag. However, mutual close encounters of the planetesimals increase eccentricities and inclinations until an equilibrium between stirring and damping is reached. After disc dissipation there is no more gas that damps the motion and mutual close encounters as well as encounters with planets stir the orbit

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Meiron, Yohai. "Expansion techniques for collisionless stellar dynamical simulations." Proceedings of the International Astronomical Union 10, S312 (2014): 227–30. http://dx.doi.org/10.1017/s1743921315007851.

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AbstractWe present ETICS, a collisionless N-body code based on two kinds of series expansions of the Poisson equation, implemented for graphics processing units (GPUs). The code is publicly available and can be used as a standalone program or as a library (an AMUSE plugin is included). One of the two expansion methods available is the self-consistent field (SCF) method, which is a Fourier-like expansion of the density field in some basis set; the other is the multipole expansion (MEX) method, which is a Taylor-like expansion of the Green's function. MEX, which has been advocated in the past, h

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Küpper, Andreas H. W., Akram H. Zonoozi, Hosein Haghi, et al. "Dynamical Evolution of Outer-Halo Globular Clusters." Proceedings of the International Astronomical Union 12, S316 (2015): 257–58. http://dx.doi.org/10.1017/s1743921315009084.

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AbstractOuter-halo globular clusters show large half-light radii and flat stellar mass functions, depleted in low-mass stars. Using N-body simulations of globular clusters on eccentric orbits within a Milky Way-like potential, we show how a cluster’s half-mass radius and its mass function develop over time. The slope of the central mass function flattens proportionally to the amount of mass a cluster has lost, and the half-mass radius grows to a size proportional to the average strength of the tidal field. The main driver of these processes is mass segregation of dark remnants. We conclude tha

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BROWN, RAY, ROBERT BEREZDIVIN, and LEON O. CHUA. "CHAOS AND COMPLEXITY." International Journal of Bifurcation and Chaos 11, no. 01 (2001): 19–26. http://dx.doi.org/10.1142/s0218127401001992.

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In this paper we show how to relate a form of high-dimensional complexity to chaotic and other types of dynamical systems. The derivation shows how "near-chaotic" complexity can arise without the presence of homoclinic tangles or positive Lyapunov exponents. The relationship we derive follows from the observation that the elements of invariant finite integer lattices of high-dimensional dynamical systems can, themselves, be viewed as single integers rather than coordinates of a point in n-space. From this observation it is possible to construct high-dimensional dynamical systems which have pro

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KELLERER, HANS G., and G. WINKLER. "RANDOM DYNAMICAL SYSTEMS ON ORDERED TOPOLOGICAL SPACES." Stochastics and Dynamics 06, no. 03 (2006): 255–300. http://dx.doi.org/10.1142/s0219493706001797.

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Let (Xn, n ≥ 0) be a random dynamical system and its state space be endowed with a reasonable topology. Instead of completing the structure as common by some linearity, this study stresses — motivated in particular by economic applications — order aspects. If the underlying random transformations are supposed to be order-preserving, this results in a fairly complete theory. First of all, the classical notions of and familiar criteria for recurrence and transience can be extended from discrete Markov chain theory. The most important fact is provided by the existence and uniqueness of a locally

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Lüghausen, Fabian, Benoit Famaey, and Pavel Kroupa. "Phantom of RAMSES (POR): A new Milgromian dynamics N-body code." Canadian Journal of Physics 93, no. 2 (2015): 232–41. http://dx.doi.org/10.1139/cjp-2014-0168.

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Since its first formulation in 1983, Milgromian dynamics (MOND) has been very successful in predicting the gravitational potential of galaxies from the distribution of baryons alone, including general scaling relations and detailed rotation curves of large statistical samples of individual galaxies covering a large range of masses and sizes. Most predictions, however, rely on static models, and only a handful of N-body codes have been developed over the years to investigate the consequences of the Milgromian framework for the dynamics of complex evolving dynamical systems. In this work, we pre

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HORVÁTHY, P. A. "DYNAMICAL (SUPER)SYMMETRIES OF MONOPOLES AND VORTICES." Reviews in Mathematical Physics 18, no. 03 (2006): 329–47. http://dx.doi.org/10.1142/s0129055x06002668.

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The dynamical (super)symmetries for various monopole systems are reviewed. For a Dirac monopole, non-smooth Runge–Lenz vector can exist; there is, however, a spectrum-generating conformal o(2,1) dynamical symmetry that extends into osp(1/1) or osp(1/2) for spin 1/2 particles. Self-dual 't Hooft–Polyakov-type monopoles admit an su(2/2) dynamical supersymmetry algebra, which allows us to reduce the fluctuation equation to the spin 0 case. For large r, the system reduces to a Dirac monopole plus a suitable inverse-square potential considered before by McIntosh and Cisneros, and by Zwanziger in th

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Yuan, Jian, Dennis L. Hartmann, and Robert Wood. "Dynamic Effects on the Tropical Cloud Radiative Forcing and Radiation Budget." Journal of Climate 21, no. 11 (2008): 2337–51. http://dx.doi.org/10.1175/2007jcli1857.1.

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Abstract Vertical velocity is used to isolate the effect of large-scale dynamics on the observed radiation budget and cloud properties in the tropics, using the methodology suggested by Bony et al. Cloud and radiation budget quantities in the tropics show well-defined responses to the large-scale vertical motion at 500 hPa. For the tropics as a whole, the ratio of shortwave to longwave cloud forcing (hereafter N) is about 1.2 in regions of upward motion, and increases to about 1.9 in regions of strong subsidence. If the analysis is restricted to oceanic regions with SST &gt; 28°C, N does n

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McMillan, Stephen L. W. "Star Cluster Simulations Including Stellar Evolution." Symposium - International Astronomical Union 208 (2003): 131–44. http://dx.doi.org/10.1017/s0074180900207092.

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The past few years have seen dramatic improvements in the scope and realism of star cluster simulations. Accurate treatments of stellar evolution, coupled with robust descriptions of all phases of binary evolution, have been incorporated self-consistently into several dynamical codes, allowing for the first time detailed study of the interplay between stellar dynamics and stellar physics. The coupling between evolution, dynamics, and the observational appearance of the cluster is particularly strong in young systems and those containing large numbers of primordial binary systems, and important

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Gemmrich, J., and C. Garrett. "Dynamical and statistical explanations of observed occurrence rates of rogue waves." Natural Hazards and Earth System Sciences 11, no. 5 (2011): 1437–46. http://dx.doi.org/10.5194/nhess-11-1437-2011.

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Abstract. Extreme surface waves occur in the tail of the probability distribution. Their occurrence rate can be displayed effectively by plotting ln(–ln P), where P is the probability of the wave or crest height exceeding a particular value, against the logarithm of that value. A Weibull distribution of the exceedance probability, as proposed in a standard model, then becomes a straight line. Earlier North Sea data from an oil platform suggest a curved plot, with a higher occurrence rate of extreme wave and crest heights than predicted by the standard model. The curvature is not accounted for

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Chardin, Jonathan, та Paolo Bianchini. "Predicting images for the dynamics of stellar clusters (π-DOC): a deep learning framework to predict mass, distance, and age of globular clusters". Monthly Notices of the Royal Astronomical Society 504, № 4 (2021): 5656–70. http://dx.doi.org/10.1093/mnras/stab737.

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ABSTRACT Dynamical mass estimates of simple systems such as globular clusters (GCs) still suffer from up to a factor of 2 uncertainty. This is primarily due to the oversimplifications of standard dynamical models that often neglect the effects of the long-term evolution of GCs. Here, we introduce a new approach to measure the dynamical properties of GCs, based on the combination of a deep-learning framework and the large amount of data from direct N-body simulations. Our algorithm, π-DOC (Predicting Images for the Dynamics Of stellar Clusters) is composed of two convolutional networks, trained

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Li, Xu, Jarken Esimbek, Jianjun Zhou, et al. "Molecular environs and triggered star formation around the large Galactic infrared bubble N 24." Monthly Notices of the Royal Astronomical Society 487, no. 2 (2019): 1517–28. http://dx.doi.org/10.1093/mnras/stz1269.

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Abstract A multi-wavelength analysis of the large Galactic infrared bubble N 24 is presented in this paper in order to investigate the molecular and star-formation environment around expanding H ii regions. Using archival data from Herschel and ATLASGAL, the distribution and physical properties of the dust over the entire bubble are studied. Using the Clumpfind2d algorithm, 23 dense clumps are identified, with sizes and masses in the range 0.65–1.73 pc and 600–16 300 M⊙, respectively. To analyse the molecular environment in N 24, observations of NH3 (1,1) and (2,2) were carried out using the N

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Chen, Y. H. "Large-Scale Uncertain Systems Under Insufficient Decentralized Controllers." Journal of Dynamic Systems, Measurement, and Control 111, no. 3 (1989): 359–63. http://dx.doi.org/10.1115/1.3153061.

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We consider a class of large-scale uncertain dynamical systems under decentralized controllers. The system is composed of N interconnected subsystems which possess uncertainty. Moreover, there are uncertainties in the interconnections. If the subsystems are under sufficient decentralized controllers, the large-scale system is practically stable. As certain controllers fail, study on the conditions for total stability of partial stability to be preserved is made. It can be shown that the stability is only related to bound of uncertainty and the structure of the large-scale system. Moreover, the

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BANAKH, T., and N. NOVOSAD. "MICRO AND MACRO FRACTALS GENERATED BY MULTI-VALUED DYNAMICAL SYSTEMS." Fractals 22, no. 04 (2014): 1450012. http://dx.doi.org/10.1142/s0218348x14500121.

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Given a multi-valued function Φ : X ⊸ X on a topological space X we study the properties of its fixed fractal[Formula: see text], which is defined as the closure of the orbit Φω(*Φ) = ⋃n∈ωΦn(*Φ) of the set *Φ = {x ∈ X : x ∈ Φ(x)} of fixed points of Φ. A special attention is paid to the duality between micro-fractals and macro-fractals, which are fixed fractals [Formula: see text] and [Formula: see text] for a contracting compact-valued function Φ : X ⊸ X on a complete metric space X. With help of algorithms (described in this paper) we generate various images of macro-fractals which are dual t

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Trenti, Michele. "Dynamical Evolution of Star Clusters with Intermediate Mass Black Holes and Primordial Binaries." Proceedings of the International Astronomical Union 3, S246 (2007): 256–60. http://dx.doi.org/10.1017/s1743921308015706.

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AbstractThe evolution of a star cluster is strongly influenced by the presence of primordial binaries and of a central black hole, as dynamical interactions within the core prevents a deep core collapse under these conditions. We present the results from a large set of direct N-body simulations of star clusters that include an intermediate mass black hole, single and binary stars. We highlight the structural and dynamical differences for the various cases showing in particular that on a timescale of a few relaxation times the density profile of the star cluster does no longer depend on the det

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SRINIVASAN, K. "MULTIPLE PERIOD DOUBLING BIFURCATION ROUTE TO CHAOS IN PERIODICALLY PULSED MURALI–LAKSHMANAN–CHUA (MLC) CIRCUIT." International Journal of Bifurcation and Chaos 18, no. 02 (2008): 541–55. http://dx.doi.org/10.1142/s021812740802046x.

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In this paper, we study the effect of additional periodic forces in Murali–Lakshmanan–Chua (MLC) circuit. We show that the additional periodic forces of pulse type display novel dynamical features including multiple period doubling bifurcation route to chaos, followed by a rich variety of dynamical phenomena including enlarged periodic windows, attractor crises, distinctly modified bifurcation structures and so on. For certain types of periodic pulses, the circuit admits transcritical bifurcations preceding the onset of multiple period doubling bifurcations. We have characterized these dynamic

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Sobolenko, Margaryta, Peter Berczik, and Rainer Spurzem. "Large scale direct galaxy collision simulations with central supermassive binary black holes." Proceedings of the International Astronomical Union 10, S312 (2014): 105–8. http://dx.doi.org/10.1017/s1743921315007620.

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AbstractWe present a set of, large scale direct N-body simulations of the galaxy collision with the central Supermassive Black Hole Binary (SMBHB) system. Based on our simulations which include the accurate Post Newtonian (PN) relativistic dynamical corrections we can estimated the merging time for the real astrophysical object. Each galaxy initially was represented as a set of particles (up to N=500k) with Plummer distribution. The SMBHBs system is described using the two special high mass, i.e. “relativistic”, particles. The interaction between these two particles have an extra PN correction

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Lübken, F. J., B. Strelnikov, M. Rapp, et al. "The thermal and dynamical state of the atmosphere during polar mesosphere winter echoes." Atmospheric Chemistry and Physics 6, no. 1 (2006): 13–24. http://dx.doi.org/10.5194/acp-6-13-2006.

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Abstract. In January 2005, a total of 18 rockets were launched from the Andøya Rocket Range in Northern Norway (69° N) into strong VHF radar echoes called "Polar Mesosphere Winter Echoes" (PMWE). The echoes were observed in the lower and middle mesosphere during large solar proton fluxes. In general, PMWE occur much more seldom compared to their summer counterparts PMSE (typical occurrence rates at 69° N are 1–3% vs. 80%, respectively). Our in-situ measurements by falling sphere, chaff, and instrumented payloads provide detailed information about the thermal and dynamical state of the atmosphe

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Lübken, F. J., B. Strelnikov, M. Rapp, et al. "The thermal and dynamical state of the atmosphere during polar mesosphere winter echoes." Atmospheric Chemistry and Physics Discussions 5, no. 4 (2005): 7613–45. http://dx.doi.org/10.5194/acpd-5-7613-2005.

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Abstract. In January 2005, a total of 18 rockets were launched from the Andøya Rocket Range in Northern Norway (69° N) into strong VHF radar echoes called 'Polar Mesosphere Winter Echoes' (PMWE). The echoes were observed in the lower and middle mesosphere during large solar proton fluxes. In general, PMWE are much more seldom compared to their summer counterparts PMSE (typical occurrence rates at 69° N are 1–3% vs. 80%, respectively). Our in-situ measurements by falling sphere, chaff, and instrumented payloads provide detailed information about the thermal and dynamical state of the atmosphere

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Li, Qiaoping, Song Yang, Tongwen Wu, and Xiangwen Liu. "Subseasonal Dynamical Prediction of East Asian Cold Surges." Weather and Forecasting 32, no. 4 (2017): 1675–94. http://dx.doi.org/10.1175/waf-d-16-0209.1.

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Abstract Predictability of East Asian cold surges is studied using daily data from the hindcasts of 45-day integrations by the NCEP Climate Forecast System version 2 (CFSv2). Prediction skills of the CFSv2 in forecasting cold surges, their annual variation, and their physical links to large-scale atmospheric circulation patterns are examined. Results show that the climatological characteristics of the East Asian winter monsoon can be reasonably reproduced by the CFSv2. The model can well capture the frequency, intensity, and location of cold surges at a lead time of about two weeks. Obviously,

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Foti, Caterina, Teiko Heinosaari, Sabrina Maniscalco, and Paola Verrucchi. "Whenever a quantum environment emerges as a classical system, it behaves like a measuring apparatus." Quantum 3 (August 26, 2019): 179. http://dx.doi.org/10.22331/q-2019-08-26-179.

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We study the dynamics of a quantum system Γ with an environment Ξ made of N elementary quantum components. We aim at answering the following questions: can the evolution of Γ be characterized by some general features when N becomes very large, regardless of the specific form of its interaction with each and every component of Ξ? In other terms: should we expect all quantum systems with a macroscopic environment to undergo a somehow similar evolution? And if yes, of what type? In order to answer these questions we use well established results from large-N quantum field theories, particularly re

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Petersen, Michael S., and Jorge Peñarrubia. "Reflex motion in the Milky Way stellar halo resulting from the Large Magellanic Cloud infall." Monthly Notices of the Royal Astronomical Society: Letters 494, no. 1 (2020): L11—L16. http://dx.doi.org/10.1093/mnrasl/slaa029.

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ABSTRACT We present the results of N-body models of the Milky Way and Large Magellanic Cloud system and study the kinematic reflex motion in the stellar halo owing to the barycentre displacement of the disc. In agreement with previous studies, we find that the Milky Way disc may be moving at 40 $\, {\rm km~s^{-1}}$ relative to the barycentre prior to the Large Magellanic Cloud infall. The resulting reflex motion is visible in tangential velocities of the stellar halo as a simple dipole. The signal is strongest for stars with long dynamical times, identifiable in position-velocity data as stars

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Bonatsos, D., E. A. McCutchan, and R. F. Casten. "What can we learn from the Interacting Boson Model in the limit of large boson numbers?" HNPS Proceedings 16 (January 1, 2020): 1. http://dx.doi.org/10.12681/hnps.2575.

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Over the years, studies of collective properties of medium and heavy mass nuclei in the framework of the Interacting Boson Approximation (IBA) model have focused on finite boson numbers, corresponding to valence nucleon pairs in specific nuclei. Attention to large boson numbers has been motivated by the study of shape/phase transitions from one limiting symmetry of IBA to another, which become sharper in the large boson number limit, revealing in parallel regularities previously unnoticed, although they survive to a large extent for finite boson numbers as well. Several of these regularities w

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Menzala, G. P., and A. F. Pazoto. "Uniform boundary stabilization of the dynamical von Kármán and Timoshenko equations for plates." Proceedings of the Royal Society of Edinburgh: Section A Mathematics 136, no. 2 (2006): 385–413. http://dx.doi.org/10.1017/s0308210500004625.

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The full nonlinear dynamic von Kárm´n system depending on a small parameter ε > 0 is considered. We study the asymptotic behaviour of the total energy associated with the model for large t and ε → 0. Introducing appropriate boundary feedback, we show that the total energy of a solution of the corresponding damped model decays exponentially as t → +∞, uniformly with respect to the parameter ε > 0. As ε → 0, we obtain a damped plate model for which the energy also tends to zero exponentially. The limit system can be viewed as new variant of the so-called Timoshenko model. It consists of a

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Vandenberg, J. M. "Interfaces and Strain in InGaAsP/InP Heterostructures Assessed with Dynamical Simulations of High-Resolution X-ray Diffraction Curves." Advances in X-ray Analysis 38 (1994): 175–80. http://dx.doi.org/10.1154/s0376030800017778.

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Abstract The interfacial structure of a lattice-matched InGaAs/InP/(100)InP superlattice with a long period of ∼630Å has been studied by fully dynamical simulations of high-resolution x-ray diffraction curves. This structure exhibits a very symmetrical x-ray pattern enveloping a large number of closely spaced satellite intensities with pronounced maxima and minima. It appears in the dynamical analysis that the position and shape of these maxima and minima is extremely sensitive to the number N of molecular layers and atomic spacing d of the InGaAs and InP layer and in particular the presence o

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TERAO, HARUHIKO. "ERG AND SCHWINGER-DYSON EQUATIONS – COMPARISON IN FORMULATIONS AND APPLICATIONS –." International Journal of Modern Physics A 16, no. 11 (2001): 1913–25. http://dx.doi.org/10.1142/s0217751x01004566.

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The advantageous points of ERG in applications to non-perturbative analyses of quantum field theories are discussed in comparison with the Schwinger-Dyson equations. First we consider the relation between these two formulations specially by examining the large N field theories. In the second part we study the phase structure of dynamical symmetry breaking in three dimensional QED as a typical example of the practical application.

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Tiongco, Maria A., Enrico Vesperini, and Anna Lisa Varri. "Kinematical evolution of Globular Clusters." Proceedings of the International Astronomical Union 14, S351 (2019): 524–27. http://dx.doi.org/10.1017/s1743921319009207.

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AbstractWe present several results of the study of the evolution of globular clusters’ internal kinematics, as driven by two-body relaxation and the interplay between internal angular momentum and the external Galactic tidal field. Via a large suite of N-body simulations, we explored the three-dimensional velocity space of tidally perturbed clusters, by characterizing their degree of velocity dispersion anisotropy and their rotational properties. These studies have shown that a cluster’s kinematical properties contain distinct imprints of the cluster’s initial structural properties, dynamical

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Nordström, Birgitta, Joss Bland-Hawthorn, Rosemary Wyse, et al. "DIVISION H COMMISSION 33: STRUCTURE & DYNAMICS OF THE GALACTIC SYSTEM." Proceedings of the International Astronomical Union 11, T29A (2015): 495–99. http://dx.doi.org/10.1017/s1743921316000946.

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Research on the structure and dynamics of the Galactic System covers a large field of research, from formation scenarios to long-term evolution and secular processes. Today we speak of near-field cosmology where the oldest parts of the Galaxy are used to probe back to early times, e.g. studying the chemical signatures of the oldest star clusters and dwarf galaxies to learn about the byproducts of the first stars. Some of the most detailed work relates to the structure of the dark matter and baryons in order to compare with expectation from N-body models. Secular processes have been identified

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Mishra, S. K., M. A. Taylor, R. D. Nair, H. M. Tufo, and J. J. Tribbia. "Performance of the HOMME dynamical core in the aqua-planet configuration of NCAR CAM4: equatorial waves." Annales Geophysicae 29, no. 2 (2011): 221–27. http://dx.doi.org/10.5194/angeo-29-221-2011.

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Abstract. A new atmospheric dynamical core, named the High Order Method Modeling Environment (HOMME), has been recently included in the NCAR-Community Climate System Model version 4 (CCSM4). It is a petascale capable high-order element-based conservative dynamical core developed on a cubed-sphere grid. We have examined the model simulations with HOMME using the aqua-planet mode of CAM4 (atmospheric component of CCSM4) and evaluated its performance in simulating the equatorial waves, considered a crucial element of climate variability. For this we compared the results with two other established

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FRIEDMANN, TAMAR. "ON BARYON NUMBER NONCONSERVATION IN TWO-DIMENSIONAL O(2N+1) QCD." International Journal of Modern Physics A 25, no. 06 (2010): 1253–66. http://dx.doi.org/10.1142/s0217751x10047853.

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We construct a classical dynamical system whose phase space is a certain infinite-dimensional Grassmannian manifold, and propose that it is equivalent to the large N limit of two-dimensional QCD with an O (2N+1) gauge group. In this theory, we find that baryon number is a topological quantity that is conserved only modulo 2. We also relate this theory to the master field approach to matrix models.

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van Albada, T. S. "N-Body Simulations of Elliptical Galaxies." Symposium - International Astronomical Union 127 (1987): 291–99. http://dx.doi.org/10.1017/s0074180900185250.

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N-body simulations are a useful tool for constructing equilibrium models of elliptical galaxies and for the exploration of their kinematical properties, in particular the tumbling rate of the figure about some axis and the internal streaming. As yet little is known about these, except that there is a large variety of possible equilibrium models. It is easy to make triaxial systems that tumble about the short axis, with internal streaming aligned with the rotation axis of the figure. Attempts to construct systems with figure rotation and internal streaming in opposite directions have not been s

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de Grijs, Richard, Chengyuan Li, and Aaron M. Geller. "The dynamical importance of binary systems in young massive star clusters." Proceedings of the International Astronomical Union 12, S316 (2015): 222–27. http://dx.doi.org/10.1017/s1743921315009096.

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AbstractCharacterization of the binary fractions in star clusters is of fundamental importance for many fields in astrophysics. Observations indicate that the majority of stars are found in binary systems, while most stars with masses greater than 0.5M⊙ are formed in star clusters. In addition, since binaries are on average more massive than single stars, in resolved star clusters these systems are thought to be good tracers of (dynamical) mass segregation. Over time, dynamical evolution through two-body relaxation will cause the most massive objects to migrate to the cluster center, while the

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Kehoe, Ryan M., Mark A. Boothe, and Russell L. Elsberry. "Dynamical Tropical Cyclone 96- and 120-h Track Forecast Errors in the Western North Pacific." Weather and Forecasting 22, no. 3 (2007): 520–38. http://dx.doi.org/10.1175/waf1002.1.

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Abstract The Joint Typhoon Warning Center has been issuing 96- and 120-h track forecasts since May 2003. It uses four dynamical models that provide guidance at these forecast intervals and relies heavily on a consensus of these four models in producing the official forecast. Whereas each of the models has skill, each occasionally has large errors. The objective of this study is to provide a characterization of these errors in the western North Pacific during 2004 for two of the four models: the Navy Operational Global Atmospheric Prediction System (NOGAPS) and the U.S. Navy’s version of the Ge

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