Numerical self-consistent stellar models of thin disks

Abstract

We find a numerical self-consistent stellar model by finding the distribution function of a thin disk that satisfies simultaneously the Fokker-Planck and Poisson equations. The solution of the Fokker-Planck equation is found by a direct numerical solver using finite differences and a variation of Stone's method. The collision term in the Fokker-Planck equation is found using the local approximation and the Rosenbluth potentials. The resulting diffusion coefficients are explicitly evaluated using a Maxwellian distribution for the field stars. As a paradigmatic example, we apply the numerical formalism to find the distribution function of a Kuzmin-Toomre thin disk. This example is studied in some detail showing that the method applies to a large family of actual galaxies.

12 pages, 9 figures, version accepted in Astronomy & Astrophysics

References in corpus (3)

• Exact General Relativistic Perfect Fluid Disks with Halos
• On the Stability of Circular Orbits of Particles Moving around Black Holes Surrounded by Axially Symmetric Structures
• On the stability of general relativistic geometric thin disks

Cited by in corpus (4)

• Stability of general relativistic static thick disks: the isotropic Schwarzschild thick disk
• Simple pairs potential-density for flat rings
• Solving procedure for a twenty-five diagonal coefficient matrix: direct numerical solutions of the three dimensional linear Fokker-Planck equation
• Stability of general relativistic Miyamoto-Nagai galaxies