# Effects of coplanar satellite bands on galactic disc evolution

**Authors:** Alexander Criswell, Curtis Struck

arXiv: 1905.13261 · 2019-06-26

## TL;DR

This study demonstrates that coplanar, corotating dwarf satellite structures can significantly influence galactic disc evolution by driving spiral waves and thickening the disc, challenging previous assumptions about their minimal impact.

## Contribution

The paper reveals that low-mass dwarf satellites in coplanar, corotating structures can induce spiral waves and disc thickening, highlighting a new mechanism for galactic evolution.

## Key findings

- Coplanar satellite structures can drive persistent spiral waves.
- Repeated satellite alignments emulate larger satellite effects.
- Disc thickening occurs due to satellite alignments.

## Abstract

Small dwarf companions have been long thought to have minimal influence on their host galaxy's evolution without undergoing direct impacts to the host's disc. However, in light of recent discoveries of coplanar, corotating satellite structures around the Milky Way, Andromeda, and Centaurus A, we use an N-body/test particle simulation to show that low-mass dwarf satellites within such structures are able to exert significant influence on their host's disc, driving spiral waves and inducing stellar scattering. This is accomplished through quasi-periodic alignments of multiple small satellites within the structure that emulate the gravitational influence of a single, larger satellite such as Sagittarius Dwarf or the Large Magellanic Cloud. We find that the coplanar, corotational nature of such structures allows for repeated alignments on short enough timescales to overcome damping within the disc, and in a consistent enough fashion to continually drive spiral waves over the course of 2 Gyr of simulation time. The spirals driven by this phenomenon tend to be flocculent and many-armed due to the irregular intervals over which alignments occur. We additionally find that while the aligned satellites are able to induce noticeable thickening of the disc, their ability to drive surface density profile evolution is secondary to other effects.

## Full text

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## Figures

25 figures with captions in the complete paper: https://tomesphere.com/paper/1905.13261/full.md

## References

23 references — full list in the complete paper: https://tomesphere.com/paper/1905.13261/full.md

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Source: https://tomesphere.com/paper/1905.13261