The limit behavior of the evolution of Tsallis entropy in self-gravitating systems

Abstract

In this letter, we study the limit behavior of the evolution of Tsallis entropy in self-gravitating systems. The study is carried out under two different situations, drawing the same conclusion. No matter in the energy transfer process or in the mass transfer process inside the system, when nonextensive parameter q is more than unity, the total entropy is bounded; on the contrary, when this parameter is less than unity, the total entropy is unbounded. There are proofs in both theory and observation that the q is always more than unity. So the Tsallis entropy in self-gravitating system generally exhibits a bounded property. This indicates the existence of global maximum of Tsallis entropy. It is possible for self-gravitating systems to evolve to thermodynamically stable states.

References in corpus (11)

• Nonextensivity in nonequilibrium plasma systems with Coulombian long-range interactions
• Nonextensive Thermostatistics and the H-Theorem
• The nonextensive parameter and Tsallis distribution for self-gravitating systems
• A nonextensive entropy approach to solar wind intermittency
• Nonextensivity and the power-law distributions for the systems with self-gravitating long-range interactions
• Non-gaussian statistics and stellar rotational velocities of main sequence field stars
• Nonextensive theory of dark matter and gas density profiles
• The nonextensive parameter for nonequilibrium plasmas in magnetic field
• A nonextensive approach to the stellar rotational evolution I. F and G type stars
• Nonextensivity in the Solar Neighborhood
• The stationary state and gravitational temperature in a pure self-gravitating system

Cited by in corpus (4)

• Effect of magnetic field on viscosity in the weakly ionized and magnetized plasma with power-law q-distributions in nonextensive statiostics
• Black Hole Thermodynamics via Tsallis Statistical Mechanics
• Tsallis $\delta$-entropy in an accelerating BIon
• $q$-Equilibrium of Gas in Spacetime of Multi-horizon Black Holes