Regular and chaotic orbits in axisymmetric stellar systems

TL;DR

This paper investigates the prevalence of chaotic and resonantly trapped orbits in axisymmetric galaxy models, quantifies their contributions, and finds that chaotic orbits are generally a very small fraction of the stellar system.

Contribution

It introduces a method to quantify the mass fractions of chaotic and resonantly trapped orbits in axisymmetric stellar systems, with applications to galaxy dynamics.

Findings

Chaotic orbits are present in all studied axisymmetric potentials.

Chaotic orbits constitute a very small fraction (~0.01% to 0.1%) of the stellar mass.

Resonantly trapped orbits are more common, comprising up to 10% of the mass.

Abstract

The gravitational potentials of realistic galaxy models are in general non-integrable, in the sense that they admit orbits that do not have three independent isolating integrals of motion and are therefore chaotic. However, if chaotic orbits are a small minority in a stellar system, it is expected that they have negligible impact on the main dynamical properties of the system. In this paper we address the question of quantifying the importance of chaotic orbits in a stellar system, focusing, for simplicity, on axisymmetric systems. Chaotic orbits have been found in essentially all (non-St\"ackel) axisymmetric gravitational potentials in which they have been looked for. Based on the analysis of the surfaces of section, we add new examples to those in the literature, finding chaotic orbits, as well as resonantly trapped orbits among regular orbits, in Miyamoto-Nagai, flattened logarithmic and shifted Plummer axisymmetric potentials. We define the fractional contributions in mass of chaotic ($\xi_{\rm c}$) and resonantly trapped ($\xi_{\rm t}$) orbits to a stellar system of given distribution function, which are very useful quantities, for instance in the study of the dispersal of stellar streams of galaxy satellites. As a case study, we measure $\xi_{\rm c}$ and $\xi_{\rm t}$ in two axisymmetric stellar systems obtained by populating flattened logarithmic potentials with the Evans ergodic distribution function, finding $\xi_{\rm c}\sim 10^{-4}-10^{-3}$ and $\xi_{\rm t}\sim 10^{-2}-10^{-1}$.