Modelling the formation of the galactic bulge

TL;DR

This study models the formation of the Galactic bulge using a Hernquist profile and chemical evolution, revealing metallicity gradients that match observations.

Contribution

It introduces a combined dynamical and chemical evolution model to explain the metallicity distribution in the Galactic bulge.

Findings

Inner bulge regions have more metal-poor stars.

Metallicity fraction decreases outward in the bulge.

Results align with observed metallicity gradients.

Abstract

In this work we have assumed a Hernquist model with an inside-out formation for the Galactic bulge and, using a chemical evolution model, we were able obtain the bulge metallicity distribution function (MDF) for different radial regions. The preliminary results show that in the inner regions of the bulge the MDF has a higher fraction of metal poor stars, while this fraction is progressively diminished as moving outwards in the bulge. These results may explain the metallicity gradient observed in the Galactic bulge.