Power Law Stellar Distributions
arXiv:astro-ph/0406404 · doi:10.1016/j.physa.2004.10.042
Abstract
The density profiles and other quantities of physical interest for spherically symmetric systems are computed by assuming that a collisionless stellar gas may relax to the non-Gaussian power law distribution suggested by the nonextensive kinetic theory. There are two different classes of solutions. The first class behaves like a subset of the polytropic Lane-Emden spheres, whereas the second one corresponds to a transition between two different polytropic indices. Unlike the isothermal Maxwellian sphere, the total mass and sizes of both classes are finite for a large range of the nonextensive q-parameter.
16 pages, 6 figures
Cited by in corpus (17)
- Simulated Dark-Matter Halos as a Test of Nonextensive Statistical Mechanics
- Nonextensivity and the power-law distributions for the systems with self-gravitating long-range interactions
- Dark matter distribution function from non-extensive statistical mechanics
- Constraining nonextensive statistics with plasma oscillation data
- Non-extensive statistics and the stellar polytrope index
- Relativity, nonextensivity, and extended power law distributions
- Nonextensive aspects of small-world networks
- Stellar polytropes and Navarro-Frenk-White halo models: comparison with observations
- Conservative Force Fields in Non-Gaussian Statistics
- The principle of maximum entropy explains the cores observed in the mass distribution of dwarf galaxies
- Numerical simulations of dark matter haloes produce polytropic central cores when reaching thermodynamic equilibrium
- Chandrasekhar's Dynamical Friction and non-extensive statistics
- Rotation Curves and Nonextensive Statistics
- On the power-law q-distribution function based on the probabilistically independent postulate in nonextensive statistics
- Constraining the Nonextensive Mass Function of Halos from BAO, CMB and X-ray data
- Brownian motion of black holes in stellar systems with non-Maxwellian distribution for the stars field
- Physically motivated fit to mass surface density profiles observed in galaxies