On the nature of buckling instability in galactic bars
Ewa L. Lokas

TL;DR
This paper investigates the buckling instability in galactic bars, revealing it occurs in two phases driven by vertical resonance, leading to a boxy/peanut shape, and clarifies it is not caused by fire-hose instability.
Contribution
The study provides a detailed simulation-based explanation of the two-phase buckling process in galactic bars, emphasizing the role of vertical resonance and pattern speed evolution.
Findings
Buckling occurs in two distinct phases with different pattern speeds.
Vertical resonance causes the initial vertical distortion and bar weakening.
The process is not related to fire-hose instability, but driven by vertical resonance.
Abstract
Many strong simulated galactic bars experience buckling instability, which manifests itself as a vertical distortion out of the disk plane, and later dissipates. Using a simulation of an isolated Milky Way-like galaxy, I demonstrate that the phenomenon can be divided into two distinct phases. In the first one, the distortion grows and its pattern speed remains equal to the pattern speed of the bar, so that the distortion remains stationary in the reference frame of the bar. The growth can be described with the mechanism of a driven harmonic oscillator with time-dependent force, which decreases the vertical frequencies of the stars. At the end of this phase, most bar-supporting orbits have banana-like shapes with a resonant vertical-to-horizontal frequency ratio close to two. The increase of amplitudes of vertical oscillations leads to the decrease of the amplitudes of horizontal…
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Taxonomy
TopicsStructural Analysis and Optimization
