Titlebook: Galactic Dynamics and N-Body Simulations; Lectures Held at the G. Contopoulos,N. K. Spyrou,L. Vlahos Conference proceedings 1994 Springer-V

Sparkle

書目名稱Galactic Dynamics and N-Body Simulations影響因子(影響力)




書目名稱Galactic Dynamics and N-Body Simulations影響因子(影響力)學科排名




書目名稱Galactic Dynamics and N-Body Simulations網絡公開度




書目名稱Galactic Dynamics and N-Body Simulations網絡公開度學科排名




書目名稱Galactic Dynamics and N-Body Simulations被引頻次




書目名稱Galactic Dynamics and N-Body Simulations被引頻次學科排名




書目名稱Galactic Dynamics and N-Body Simulations年度引用




書目名稱Galactic Dynamics and N-Body Simulations年度引用學科排名




書目名稱Galactic Dynamics and N-Body Simulations讀者反饋




書目名稱Galactic Dynamics and N-Body Simulations讀者反饋學科排名

AMOR

978-3-662-13982-0Springer-Verlag Berlin Heidelberg 1994

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昏暗

reptile

A. Dukat,P. Gavornik,J. Kolesar,Z. Mikes degrees of freedom. Then we discuss integrable systems in general. In particular we consider Li ouville systems and the Painlevé test of integrability. Formal integrals (like the “third” integral) are an important tool in galactic dynamics. We discuss their construction, and the limits of their app

范圍廣

Wladislaw Rivkin,Klaus-Helmut Schmidtls of spiral galaxies and the comparison with observations yield important information on the basic state of such systems which otherwise cannot be obtained. Normal, grand design spirals are emphasized because they show many of the basic dynamic effects more clearly. The morphology of spiral galaxie

范圍廣

Jan Terhoeven,Sascha Wischniewskions feasible. We demonstrate this using the study of linear normal modes of spherical stellar systems as a paradigm. We explore the limitations of numerical simulations using various techniques and advocate the use of smooth potential codes as ideally suited to this problem. We discuss three instabi

恩惠

M. Parini,H. Scriba,C. Sieber,D. Wernerndividual time-steps. The new Hermite integration scheme is described; it is based on explicit evaluation of the force and its first derivative. We show that this scheme is particularly efficient when combined with hierarchical time-steps which reduce the amount of prediction. Some examples of time

偏狂癥

Linda K. Haymes,Debra L. Cote,Keith Storeyical equations by means of finite-difference schemes are discussed together with the errors and problems arising during this process. An alternative solution method, called Smoothed Particle Hydrodynamics, is also discussed. Finally, two applications concerning the evolution of clusters of galaxies

Carcinoma

Qingxu Jin,Christopher K. Y. Leungblem, is briefly presented in the introduction. Section 2 deals with the properties of density perturbations. The emphasis is given on describing the role of the power spectrum of density perturbations in constructing the typical mass fluctuations of various mass scales. The evolution of a density p