Three-dimensional galaxy simulations

Abstract

A three-dimensional fully self-consistent computer model was used to determine the evolution of galaxies consisting of 100,000 simulation stars with exponential radial density variation. Comparison with two-dimensional (infinitesimally thin disk) simulations showed only a very slight stabilizing effect due to the additional degree of freedom. The addition of a fully self-consistent, nonrotating, exponential core/halo component resulted in considerable stabilization. The most pronounced instabilities present were those due to the Jeans' instability in the outer regions of the disk, while at the same time a relatively slowly-growing bar instability appeared. The two-dimensional disk, plus core/halo simulation, showed the usual fast-growing instability leading to bar formation.