# Dynamics of thick, open spirals in Perlas potentials

## TL;DR

This study explores the three-dimensional stellar dynamics supporting open spiral arms in galaxies using the PERLAS potential, identifying orbit families that sustain spiral structures and their stability across different mass ratios.

## Contribution

It extends previous two-dimensional studies by analyzing 3D orbit families and their stability in spiral galaxy models with varying spiral-to-disk mass ratios.

## Key findings

- Optimal support for 25° pitch angle spirals occurs at M_s/M_d between 0.03 and 0.07.
- Strong spiral patterns are supported between the 2:1 and 4:1 resonances.
- A bar-like structure appears inside the 2:1 resonance in all models.

## Abstract

The PERLAS potential has been successfully used in many studies related with the dynamics of the spiral arms \textit{on} the equatorial plane of normal (non-barred) spiral galaxies. In the present work we extend these studies by investigating the three-dimensional dynamics of the spiral arms in the same type of potential. We consider a typical open, logarithmic, spiral pattern of pitch angle 25$^{\circ}$ and we examine the stellar orbits that can support it as the ratio of the masses of the spiral over the disk component ($M_{s}/M_{d}$) varies. We indicate the families of `three-dimensional' periodic orbits that act as the backbone of the spiral structure and we discuss their stability in the models we present. We study further the quasi-periodic and non-periodic orbits in general that follow spiral-supporting orbits as the $M_{s}/M_{d}$ ratio increases. We find that a bisymmetric spiral with 25$^{\circ}$ pitch angle is better supported by orbits in models with $0.03\lessapprox M_{s}/M_{d} \lessapprox 0.07$. In these cases a strong spiral pattern is supported between the radial 2:1 and 4:1 resonances, while local enhancements of the imposed spirals are encountered in some models between 4:1 and corotation. A characteristic bar-like structure is observed in all models at radii smaller than the radius of the 2:1 resonance.