# Is the late buckling stage inevitable in the bar life?

## TL;DR

This study uses numerical simulations to explore how classical bulges influence bar buckling, revealing that even modest bulges can suppress secondary buckling, potentially explaining the rarity of ongoing buckling in observed bars.

## Contribution

It demonstrates that classical bulges can prevent secondary buckling in bars, a novel insight into bar evolution and stability.

## Key findings

- Modest bulges suppress secondary buckling in bars.
- Bars without bulges experience both primary and secondary buckling.
- Classical bulges and central gas concentration may explain the scarcity of ongoing buckling.

## Abstract

By means of self-consistent numerical simulations we investigated the dynamical impact of classical bulges on the growth of the secondary buckling of a bar. Overall we considered 14 models with different disc and bulge parameters. We obtained that a bulge with a quite modest mass $B/D=0.1$ leads to completely symmetrical evolution of the bar almost independently of the initial stellar disc parameters and even can damp the first bending. At the same time, the bars in all our bulgeless models suffer from the short primary and prolonged secondary buckling. Given the smallness of the mass suppressing secondary buckling, we conclude that a classical bulge along with the gas central concentration may be the main culprits for the rarity of bars with ongoing buckling in the local Universe.