Titlebook: Ergodic Concepts in Stellar Dynamics; Proceedings of an In V. G. Gurzadyan,D. Pfenniger Conference proceedings 1994 Springer-Verlag Berlin

漠不关心

书目名称Ergodic Concepts in Stellar Dynamics影响因子(影响力)




书目名称Ergodic Concepts in Stellar Dynamics影响因子(影响力)学科排名




书目名称Ergodic Concepts in Stellar Dynamics网络公开度




书目名称Ergodic Concepts in Stellar Dynamics网络公开度学科排名




书目名称Ergodic Concepts in Stellar Dynamics被引频次




书目名称Ergodic Concepts in Stellar Dynamics被引频次学科排名




书目名称Ergodic Concepts in Stellar Dynamics年度引用




书目名称Ergodic Concepts in Stellar Dynamics年度引用学科排名




书目名称Ergodic Concepts in Stellar Dynamics读者反馈




书目名称Ergodic Concepts in Stellar Dynamics读者反馈学科排名

galley

Some clues about the dynamics of globular clusters from high-resolution observation,elescope (HST). Contrary to galaxies, whose distances are generally larger than 1 Mpc, implying unresolved stellar distributions, globular clusters have distances of the order of 10 kpc, which allow HST to resolve the brightest stars into grainy stellar distributions. We specifically discuss here so

逗它小傻瓜

Ergodic methods in stellar dynamics,eems to be the precise definitions and hence the unique meaning of the terminology and notation often used in stellar dynamics, such as ., etc..In particular, we have seen that the term . cannot necessarily be attributed only to processes which involve exchange of energy between particles. The class

canonical

Recent developments in the dynamics of nonlinear Hamiltonian systems with many degrees of freedom,f the main theoretical points of this research field are also briefly discussed and compared with the outcomes of recent numerical simulations..New results, obtained with a differential geometrical approach to Hamiltonian dynamics, are also presented together with a mention of their consequences for

是限制

Ergodicity and mixing in gravitating systems,i.e. for galaxies of the most usual types) the systems are practically collisionless for time scales not exceeding the Hubble time. So it is necessary to follow phase trajectories not only in the 6.-D phase space but in the 6-D phase space. Studying the 6.-D space will give no new information for co

音乐等

音乐等

Lyapunov analysis of stable chaos in self-gravitating many body systems,l galaxies consist of regular stellar orbits, whereas nonlinear interaction in self-gravitating many-body systems makes the elliptical galaxies chaotic. A new type of chaos, “stable chaos”, in which orbits do not change significantly although they have orbital instability (positive Lyapunov exponent

irreparable

Stability of the modified Konishi-Kaneko system,mical stability is investigated with the use of the collisionless Boltzmann equation. The predicted growth rates agree excellently with those obtained from N-body simulations..Thermodynamic arguments show that the system has clustered equilibrium states as well as uniform states for 1/. > 4./., wher

书法

Mixing transformations of N particles conserving almost all classical integrals,ct them to conserve the mass, centers of mass and velocity, and especially the total angular momentum. Furthermore, for simple linear friction laws it is possible to specify in advance the energy dissipation. In that case the conservation of the other integrals constraints the energy loss not exceed

radiograph

Discreteness noise versus force errors in N-body simulations, main result is that force calculation with a low accuracy — a few percent for each particle pair — is sufficient, irrespective of the number of particles. Higher accuracy is useless since the discreteness noise, i.e., the two-body relaxation effect, dominates the error. We have performed numerical