Formation timescales for stellar bars in diverse galactic discs

TL;DR

This study investigates how disc structure and kinematics influence the timescale of stellar bar formation in galaxies, using extensive simulations to relate stability criteria to bar growth rates across different galaxy models.

Contribution

It extends previous work by analyzing thicker, more turbulent discs and establishing empirical relations between stability criteria and bar formation timescales.

Findings

Bar formation timescales follow a power law with stability criteria.

Discs with higher velocity dispersion have delayed bar growth.

Bars form faster in live haloes compared to static haloes.

Abstract

We study the formation of stellar bars using 145 simulations of disc galaxies embedded in live and static dark matter haloes. We use the exponential bar growth timescale, $\tau_{\rm bar}$, to quantify how disc structure and kinematics regulate the onset and rate of secular bar formation. We extend previous work to thicker and more turbulent discs, motivated by those observed at high redshift ($z>1$). By revisiting several commonly used disc stability criteria - the Efstathiou-Lake-Negroponte parameter ($\epsilon_{\rm ELN}$), the Ostriker-Peebles ratio ($t_{\rm OP}$), and the disc stellar mass fraction within 2.2 disc scale radii ($f_{\rm disc}$) - we find that $\tau_{\rm bar}$, when expressed in terms of the disc's orbital period, follows a tight power law with each criteria. In Milky Way-like discs embedded in live haloes, bars form within a Hubble time if $f_{\rm disc} \geq 0.18$, $t_{\rm OP} \geq 0.27$, and $\epsilon_{\rm ELN} \leq 1.44$. We show discs with higher velocity dispersion experience delayed bar growth and introduce an empirical relation that correctly describes the bar formation timescales of all our live halo models. Bars in static haloes grow at roughly half the rate of those in live haloes and require substantially greater disc instability to do so.