Modelling the chemical evolution of the Milky Way

Abstract

In this review I will discuss the comparison between model results and observational data for the Milky Way, the predictive power of such models as well as their limits. Such a comparison, known as Galactic archaeology, allows us to impose constraints on stellar nucleosynthesis and timescales of formation of the various Galactic components (halo, bulge, thick disk and thin disk).

arXiv comment93 pages,37 figures. Accepted in Astronomy & Astrophysics Review

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• An Introduction to Galactic Chemical Evolution
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• Disk heating and stellar migration in galaxies
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• The impact of very massive stars on the chemical evolution of extremely metal-poor galaxies
• The Galactic Chemical Evolution of phosphorus observed with IGRINS
• The stellar halo in Local Group Hestia simulations III. Chemical abundance relations for accreted and in-situ stars
• Metallicity of Galactic RR Lyrae from Optical and Infrared Light Curves: II. Period-Fourier-Metallicity Relations for First Overtone RR Lyrae
• Disc dichotomy signature in the vertical distribution of [Mg/Fe] and the delayed gas infall scenario
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• Elemental abundances in M31: Individual and Coadded Spectroscopic [Fe/H] and [α/Fe] throughout the M31 Halo with SPLASH
• Study of Chemically Peculiar Stars-I : High-resolution Spectroscopy and K2 Photometry of Am Stars in the Region of M44
• GalCEM I -- An Open-Source Detailed Isotopic Chemical Evolution Code
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• Are Milky-Way-like galaxies like the Milky Way? A view from SDSS-IV/MaNGA
• ATLASGAL-selected massive clumps in the inner Galaxy. X. Observations of atomic carbon at 492 GHz
• New Fe I Level Energies and Line Identifications from Stellar Spectra. III. Initial Results from UV, Optical, and Infrared Spectra
• Neutron-capture elements record the ordered chemical evolution of the disc over time