Titlebook: Galaxies and Chaos; George Contopoulos,Nikos Voglis Book 2003 Springer-Verlag Berlin Heidelberg 2003 Celestial mechanics.Galaxy.dynamical

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Jeans Solutions for Triaxial Galaxies,ystems, there are three equations, but these are not very helpful, as they contain six independent moments. By assuming that the potential is triaxial and of separable St?ckel form, the mixed moments vanish in confocal ellipsoidal coordinates. The three Jeans equations and three remaining non-vanish

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The Level of Chaos in N-Body Models of Elliptical Galaxies,g values of the Lyapunov Characteristic Numbers) in self-consistent N-body models of elliptical galaxies. A careful simultaneous use of several numerical tools can induce the proportion of particles in chaotic orbits dynamically important within one Hubble time. In models with smooth centers the mas

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VEIL

Disk-Crossing Orbits,esent evidence that this simplifying assumption is not critical. We find that the presence of the disk causes many more resonances than have been found in similar smooth potentials. Those resonances grow at relatively modest values of energy, overlap, and give rise to many stochastic orbits. A signi

SHRIK

Chaos and Chaotic Phase Mixing in Galaxy Evolution and Charged Particle Beams,aning of chaos in many-body systems, (ii) the time-dependence of the bulk potential, which can trigger intervals of ., and (iii) the self-consistent nature of any bulk chaos, which is generated by the bodies themselves, rather than imposed externally. Simulations and theory both suggest strongly tha

GOUGE

Motions of a Black Hole near the Center of a Galaxy, as an orbiting density wave which grows near the center in a galaxy model that starts without such motions. While these experiments were run without a massive particle, we suggested that similar physical effects might cause a massive particle near the center to oscillate with larger amplitudes than

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Weak Homology of Bright Elliptical Galaxies,the Fundamental Plane reflects the existence of an underlying mass-luminosity relation for such galaxies, in a scenario where elliptical galaxies are homologous systems in dynamical equilibrium. Here I will re-examine the issue of whether empirical evidence supports the view that significant systema

macular-edema

天然熱噴泉

Observational Determination of the Gravitational Potential and Pattern Speed in Strongly Barred Galrs are difficult to determine, in particular for strongly barred galaxies. We will briefly review different methods and illustrate in more detail the case where the problem has been approached by numerical gasdynamical simulations.