Star cluster evolution in barred disc galaxies. I. Planar periodic orbits

TL;DR

This study investigates how the unique tidal effects of galactic bars influence star cluster evolution, using N-body simulations to compare different orbital configurations and their impact on cluster dissolution and tidal tail morphology.

Contribution

It introduces the first detailed analysis of star cluster evolution within barred galaxy potentials, highlighting the importance of orbit shape and stability on cluster dynamics.

Findings

Orbital shape and stability significantly affect cluster evolution.

Tidal tail morphology depends on the orbit's orientation and stability.

Cluster dissolution time is mainly influenced by tidal forcing, not potential shape.

Abstract

The dynamical evolution of stellar clusters is driven to a large extent by their environment. Several studies so far have considered the effect of tidal fields and their variations, such as, e.g., from giant molecular clouds, galactic discs, or spiral arms. In this paper we will concentrate on a tidal field whose effects on star clusters have not yet been studied, namely that of bars. We present a set of direct N-body simulations of star clusters moving in an analytic potential representing a barred galaxy. We compare the evolution of the clusters moving both on different planar periodic orbits in the barred potential and on circular orbits in a potential obtained by axisymmetrising its mass distribution. We show that both the shape of the underlying orbit and its stability have strong impact on the cluster evolution as well as the morphology and orientation of the tidal tails and the sub-structures therein. We find that the dissolution time-scale of the cluster in our simulations is mainly determined by the tidal forcing along the orbit and, for a given tidal forcing, only very little by the exact shape of the gravitational potential in which the cluster is moving.