# Gas removal in the Ursa Minor galaxy: linking hydrodynamics and chemical evolution models

## TL;DR

This study combines hydrodynamical and chemical evolution models to simulate gas loss in the Ursa Minor galaxy, highlighting supernovae and environmental effects as key drivers of gas removal.

## Contribution

It introduces a novel simulation approach that integrates supernova rates from chemical models with hydrodynamics to study gas loss in dwarf galaxies.

## Key findings

- Supernovae significantly contribute to gas loss in Ursa Minor.
- Gas loss varies over time and radius, peaking early in the galaxy's evolution.
- Environmental effects like ram-pressure stripping also play a crucial role.

## Abstract

We present results from a non-cosmological, three-dimensional hydrodynamical simulation of the gas in the dwarf spheroidal galaxy Ursa Minor. Assuming an initial baryonic-to-dark-matter ratio derived from the cosmic microwave background radiation, we evolved the galactic gas distribution over 3 Gyr, taking into account the effects of the types Ia and II supernovae. For the first time, we used in our simulation the instantaneous supernovae rates derived from a chemical evolution model applied to spectroscopic observational data of Ursa Minor. We show that the amount of gas that is lost in this process is variable with time and radius, being the highest rates observed during the initial 600 Myr in our simulation. Our results indicate that types Ia and II supernovae must be essential drivers of the gas loss in Ursa Minor galaxy (and probably in other similar dwarf galaxies), but it is ultimately the combination of galactic winds powered by these supernovae and environmental effects (e.g., ram-pressure stripping) that results in the complete removal of the gas content.