# Dynamics and Morphology of the Milky Way Spiral Arms from the Metallicity Distribution and Radial Mixing

## TL;DR

This study investigates how the metallicity distribution function (MDF) and radial migration influence the structure and evolution of the Milky Way's spiral arms, providing new constraints on galactic dynamics and chemical evolution.

## Contribution

It introduces a detailed chemical tagging method in simulations to constrain spiral arm parameters and assesses the impact of radial migration on metallicity gradients over time.

## Key findings

- The MDF reveals information about spiral structure and radial migration.
- The Sun likely formed away from its current galactocentric position.
- The Milky Way's metallicity gradient remains largely intact despite radial mixing.

## Abstract

Albeit radial migration must be a ubiquitous process in disc galaxies, its significance in the evolution of stellar discs is not always reflected through global trends. However, there are other key observables, such as the metallicity distribution function (MDF), that may shed some light in this matter. We argue that the shape of the MDF not only tells us whether the stellar disc experienced radial migration, but it also contains important clues on the structure that triggered it. Specifically, the MDF contains information about the dynamics and morphology of the spiral pattern. To constrain the spiral parameters, we have included a detailed chemical tagging in our simulations; this allows us to produce a restriction of the structural parameters of the spiral arms in the Milky Way as well as a method to constrain chemical evolution models towards the center of the Galactic disc, where no chemical model provides information. We also found that it is unlikely that the Sun was formed near its current galactocentric position, therefore it might be inaccurate to consider the Sun as representative of the chemical abundances in the solar neighborhood. We also show that a stellar disc of the Milky Way, after evolving dynamically and chemically for 5 Gyr, preserves 80% of its original global metallicity gradient despite having suffered important heating and radial migration; this means that the presence of a metallicity gradient in a given galaxy, does not guarantee that radial mixing has not played a role in its evolution.