Thermodynamics of rotating self-gravitating systems

Details Thermodynamics of rotating self-gravitating systems Thermodynamics of rotating self-gravitating systems

2002-07-05

arxiv.org/abs/cond-mat/0207153v1

Eur.Phys.J. B29 (2002) 593

Physics

Condensed Matter

Statistical Mechanics

12 pages, 9 figures

Scientific paper

10.1140/epjb/e2002-00317-4

We investigate the statistical equilibrium properties of a system of classical particles interacting via Newtonian gravity, enclosed in a three-dimensional spherical volume. Within a mean-field approximation, we derive an equation for the density profiles maximizing the microcanonical entropy and solve it numerically. At low angular momenta, i.e. for a slowly rotating system, the well-known gravitational collapse ``transition'' is recovered. At higher angular momenta, instead, rotational symmetry can spontaneously break down giving rise to more complex equilibrium configurations, such as double-clusters (``double stars''). We analyze the thermodynamics of the system and the stability of the different equilibrium configurations against rotational symmetry breaking, and provide the global phase diagram.

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