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Using N-body simulations to understand the chemo-dynamical evolution of the inner Milky Way

Published online by Cambridge University Press:  02 August 2018

E. Athanassoula
E. Athanassoula*
Affiliation:
Aix Marseille Univ, CNRS, LAM, Laboratoire d’Astrophysique de Marseille, Marseille, France email: lia@lam.fr
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Abstract

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I present examples of how chemo-dynamical N-body simulations can help understanding the structure and evolution of the inner Galaxy. Such simulations reproduce the observed links between kinematics, morphology and chemistry in the bar/bulge region and explain them by the self-consistent cohabitation of a number of components. Galactic archaeology, applied to simulation snapshots, explains the sequence in which the stars of the various components were formed. The thick disc stars form earlier than those of the thin disc and in a much shorter time scale. The bar in the thick disc is horizontally thicker than that of the thin disc and has a different vertical morphology. The Galaxy’s inner disc scalelength is much smaller than what is expected from nearby galaxies of similar stellar mass.

Keywords

Galaxy: bulgeGalaxy: stellar contentGalaxy: structureGalaxy: kinematics and dynamicsGalaxy: evolutiongalaxies: structure — galaxies: kinematics and dynamics — galaxies:spiral — galaxies:evolution — galaxies:evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 65 - 72
Copyright
Copyright © International Astronomical Union 2018 

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