# Tidally induced bars in dwarf galaxies on different orbits around a Milky Way-like host

## TL;DR

This study uses N-body simulations to analyze how orbital parameters influence bar formation and evolution in dwarf galaxies orbiting a Milky Way-like host, revealing that bars form during pericenter passages and their strength depends on orbit size and inclination.

## Contribution

It provides new insights into the dependence of bar formation and characteristics on orbital configuration and inclination in dwarf galaxies orbiting larger hosts.

## Key findings

- Bars form during the first pericenter passage in all cases.
- Bar strength varies with orbit size and disc inclination.
- Bars are generally slow rotators with minimal secular evolution.

## Abstract

Bars in galaxies may develop through a global instability or due to an interaction with another system. We study bar formation in disky dwarf galaxies orbiting a Milky Way-like galaxy. We employ $N$-body simulations to study the impact of initial orbital parameters: the size of the dwarf galaxy orbit and the inclination of its disc with respect to the orbital plane. In all cases a bar develops in the center of the dwarf during the first pericenter on its orbit around the host. Between subsequent pericenter passages the bars are stable, but at the pericenters they are usually weakened and shortened. The initial properties and details of the further evolution of the bars depend heavily on the orbital configuration. We find that for the exactly prograde orientation, the strongest bar is formed for the intermediate-size orbit. On the tighter orbit, the disc is too disturbed and stripped to form a strong bar. On the wider orbit, the tidal interaction is too weak. The dependence on the disc inclination is such that weaker bars form in more inclined discs. The bars experience either a very weak buckling or none at all. We do not observe any secular evolution, possibly because the dwarfs are perturbed at each pericenter passage. The rotation speed of the bars can be classified as slow ($R_\mathrm{CR}/l_\mathrm{bar}\sim2-3$). We attribute this to the loss of a significant fraction of the disc's rotation during the encounter with the host galaxy.