Regular and chaotic orbits in barred galaxies - I. Applying the SALI/GALI method to explore their distribution in several models

TL;DR

This study applies SALI/GALI methods to classify chaotic and regular orbits in barred galaxy models, revealing how orbit behavior depends on energy, position, and bar properties, with implications for galactic dynamics.

Contribution

It introduces a comprehensive application of SALI/GALI techniques to analyze orbit regularity in barred galaxy models across different dimensions and parameters.

Findings

Regular orbits are more common near the galaxy center and equatorial plane.

Chaotic orbits dominate in models with more massive bars.

The fraction of chaotic orbits correlates strongly with bar strength.

Abstract

The distinction between chaotic and regular behavior of orbits in galactic models is an important issue and can help our understanding of galactic dynamical evolution. In this paper, we deal with this issue by applying the techniques of the Smaller (and Generalized) ALingment Indices, SALI (and GALI), to extensive samples of orbits obtained by integrating numerically the equations of motion in a barred galaxy potential. We estimate first the fraction of chaotic and regular orbits for the two-degree-of-freedom (DOF) case (where the galaxy extends only in the (x,y)-space) and show that it is a non-monotonic function of the energy. For the three DOF extension of this model (in the z-direction), we give similar estimates, both by exploring different sets of initial conditions and by varying the model parameters, like the mass, size and pattern speed of the bar. We find that regular motion is more abundant at small radial distances from the center of the galaxy, where the relative non-axisymmetric forcing is relatively weak, and at small distances from the equatorial plane, where trapping around the stable periodic orbits is important. We also find that the variation of the bar pattern speed, within a realistic range of values, does not affect much the phase space's fraction of regular and chaotic motions. Using different sets of initial conditions, we show that chaotic motion is dominant in galaxy models whose bar component is more massive, while models with a fatter or thicker bar present generally more regular behavior. Finally, we find that the fraction of orbits that are chaotic correlates strongly with the bar strength.