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Galactic Chemical Evolution

Published online by Cambridge University Press:  05 March 2013

Brad K. Gibson ,
Yeshe Fenner ,
Agostino Renda ,
Daisuke Kawata  and
Hyun-chul Lee
Brad K. Gibson
Affiliation:
Centre for Astrophysics & Supercomputing, Swinburne University, Mail #31, Hawthorn, Vic 3122, Australia; bgibson@astro.swin.edu.au
Yeshe Fenner
Affiliation:
Centre for Astrophysics & Supercomputing, Swinburne University, Mail #31, Hawthorn, Vic 3122, Australia; yfenner@astro.swin.edu.au
Agostino Renda
Affiliation:
Centre for Astrophysics & Supercomputing, Swinburne University, Mail #31, Hawthorn, Vic 3122, Australia; arenda@astro.swin.edu.au
Daisuke Kawata
Affiliation:
Centre for Astrophysics & Supercomputing, Swinburne University, Mail #31, Hawthorn, Vic 3122, Australia; dkawata@astro.swin.edu.au
Hyun-chul Lee
Affiliation:
Centre for Astrophysics & Supercomputing, Swinburne University, Mail #31, Hawthorn, Vic 3122, Australia; hclee@astro.swin.edu.au
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Abstract

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The primary present-day observables upon which theories of galaxy evolution are based are a system’s morphology, dynamics, colour, and chemistry. Individually, each provides an important constraint to any given model; in concert, the four represent a fundamental (intractable) boundary condition for chemodynamical simulations. We review the current state-of-the-art semi-analytical and chemodynamical models for the Milky Way, emphasising the strengths and weaknesses of both approaches.

Keywords

Galaxy: abundancesGalaxy: evolutionGalaxy: formationGalaxy: kinematics and dynamicsmethods: N-body simulations
Type
Sixth Torino Workshop
Information
Publications of the Astronomical Society of Australia , Volume 20 , Issue 4 , 2003 , pp. 401 - 415
Copyright
Copyright © Astronomical Society of Australia 2003

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