# Stability of galaxies across morphological sequence

Source: [Stability of galaxies across morphological sequence](<https://www.sota2.com/research/paper/68fa44221e209131ce90f12f>)

Collection index: [llms.txt](<https://www.sota2.com/research/llms.txt>)

Data updated: 2025-10-25T04:38:58.125Z

Authors: K. Aditya

Published: 2023-04-16T09:21:24.000Z

## Abstract

We investigate the stability of nearby disc galaxies and galaxies at redshift ($z$) equal to 4.5. We explore the connection between the stability parameter $(Q\_{RW})$, star formation rate ($SFR$), gas fraction $(f^{Gas})$, and the time scale for growth of gravitational instabilities $(\\tau)$. We find that, despite differences in morphology $91$ $\\%$ of the nearby galaxies have a minimum value of stability parameter ($Q^{Min}\_{RW}$) greater than $1$ indicating stability against the growth of axisymmetric instabilities. The spirals in our sample have higher median star formation rate, lower median $Q\_{RW}$, a lower $f^{Gas}$ and small time scale for growth of gravitational instabilities than irregular galaxies. We find that the gravitational instabilities in spirals convert a large fraction of gas into stars quickly, depleting the gas reservoirs. On the other hand, star formation occurs more gradually over longer timescales in irregulars with a higher gas fraction. We then compare the stability of the nearby galaxies with galaxies at $z\\,=\\,4.5$. We find that net stability levels in the nearby galaxies and the galaxies at $z\\,=\\,4.5$ are primarily driven by the stellar disc suggesting the presence of an inherent mechanism that self-regulates the stability. Finally, upon removing the contribution of the dark matter to the total potential, the median $Q\_{RW}$ for the nearby galaxies and galaxies at $z \\,= \\,4.5$ remains unchanged indicating that the baryons can self-regulate the stability levels, at least in a statistical sense.

## Recorded benchmark results

A research result applies to its stated dataset, split, metric and evaluation configuration. Compare like-for-like settings, preserve the metric's unit and direction, and distinguish paper-reported results from independent reproduction. The best result recorded here is not a claim of exhaustive, current global coverage.

## Original sources and implementation

[Original paper](<https://arxiv.org/abs/2304.07734>)

[PDF](<https://arxiv.org/pdf/2304.07734.pdf>)