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Abstract
The formation of self-gravitating systems is studied by simulating the collapse of a set of N particles which are generated from several distribution functions. We first establish that the results of such simulations depend on N for small values of N. We complete a previous work by Aguilar and Merritt concerning the morphological segregation between spherical and elliptical equilibria. We find and interpret two new segregations: one concerns the equilibrium core size and the other the equilibrium temperature. All these features are used to explain some of the global properties of self-gravitating objects: origin of globular clusters and central black hole or shape of elliptical galaxies.
Highlights
It is intuitive that the gravitational collapse of a set of N masses is directly related to the formation of astrophysical structures like globular clusters or elliptical galaxies
There is no study which indicates clearly that the time dependence of the solutions disappears in a few dynamical times, giving a well defined equilibrium-like state
In the CBE context (see Perez & Aly (1998) for a review), it is well known that spherical systems are generally stable except in the case where a large radial anisotropy is present in the velocity space. This is the Radial Orbit Instability, hereafter denoted by ROI (see Perez & Aly (1998), and Perez et al (1998) for a detailed analytic and numeric study of these phenomena) which leads to a bar-like equilibrium state in a few dynamical times
Summary
It is intuitive that the gravitational collapse of a set of N masses is directly related to the formation of astrophysical structures like globular clusters or elliptical galaxies (the presence of gas may complicate the pure gravitational N -body problem for spiral galaxies). In the CBE context (see Perez & Aly (1998) for a review), it is well known that spherical systems (with decreasing spatial density) are generally stable except in the case where a large radial anisotropy is present in the velocity space This is the Radial Orbit Instability, hereafter denoted by ROI (see Perez & Aly (1998), and Perez et al (1998) for a detailed analytic and numeric study of these phenomena) which leads to a bar-like equilibrium state in a few dynamical times. Van Albada (1982) remarked that the dissipationless collapse of a clumpy cloud of N equal masses could lead to a final stationary state that is quite similar to elliptical galaxies This kind of study was reconsidered in an important work by Aguilar & Merritt (1990), with more details and a crucial remark concerning the correlation between the final shape (spherical or oblate) and the virial ratio of the initial state.
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