Self-gravitating Stellar Systems and Non-extensive Thermostatistics

Abstract

After introducing the fundamental properties of self-gravitating systems, we present an application of Tsallis' generalized entropy to the analysis of their thermodynamic nature. By extremizing the Tsallis entropy, we obtain an equation of state known as the stellar polytrope. For a self-gravitating stellar system confined within a perfectly reflecting wall, we discuss the thermodynamic instability caused by its negative specific heat. The role of the extremum as a quasi-equilibrium is also demonstrated from the results of N-body simulations.

15 pages, 8 figures, final version to apper in CMT

References in corpus (4)

• Long-term Evolution of Stellar Self-Gravitating System away from the Thermal Equilibrium: connection with non-extensive statistics
• Gravitational instability of isothermal and polytropic spheres
• Anomalous diffusion and collapse of self-gravitating Langevin particles in D dimensions
• Gravothermal Catastrophe and Tsallis' Generalized Entropy of Self-Gravitating Systems III. quasi-equilibrium structure using normalized q-values

Cited by in corpus (11)

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• Stellar polytropes and Navarro-Frenk-White halo models: comparison with observations
• Antonov problem and quasi-equilibrium states in N-body system
• Slow relaxation in the two dimensional electron plasma under the strong magnetic field
• Gamow Temperature in Tsallis and Kaniadakis Statistics
• Entropic Upper Bound on Gravitational Binding Energy
• Black Hole Thermodynamics via Tsallis Statistical Mechanics
• $q$-Equilibrium of Gas in Spacetime of Multi-horizon Black Holes