Titlebook: Stability of Collisionless Stellar Systems; Mechanisms for the D P. L. Palmer Book 1994 Springer Science+Business Media Dordrecht 1994 Cosm

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Biguanides

Description of the Orbital Motions,at the motion of individual stars within the galaxies, show how their motions are determined, and introduce different notations that will prove useful in the description of these motions. We will consider three kinds of systems in this book, spherical systems, axisymmetric systems and disc systems.

休閑

General Perturbation Theory,e the theory for a number of cases which will be of interest to us later. It is important to note that in this section we are only considering individual stars and thus we cannot infer anything about collective instability in the system, which requires a self-consistent build up of the combination o

Observe

Constructing Equilibrium Models,f because although there are a lot of models in the literature, our aim in this book is to discuss stability in general terms, rather than stability of individual models. Discussion of various equilibrium models can be found in [45] and [56]. We shall set out the general principles of model building

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雪崩

Isotropic Systems,r, discuss what we may learn from this matrix equation for stellar systems in which the pressure from random motions is isotropic. Such systems were, for a long time, thought to be the most appropriate to describe elliptical galaxies with the further restriction that their distribution function decr

賄賂

chalice

Malleable

Evacuate