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Article Contents

ABSTRACT

1.INTRODUCTION

1.1.What do we want to learn?

1.2.Some relevant observations

1.2.1.Stars

1.2.2.Gas

1.2.3.Dark matter

1.2.4.Super-massive black holes

1.2.5.The Milky Way

1.3.Learning from galaxy evolution with redshift

1.3.1.Ubiquitous winds

1.3.2.Size evolution of early-type galaxies

1.3.3.Evolution of spiral galaxies

1.3.4.Evolution of star formation rates and gas fractions

1.4.Methods of solution

1.4.1.Direct simulations of dark matter

1.4.2.Semi-analytical models for baryons

1.4.3.Direct simulations including baryons

1.5.Disks, Ellipticals and Mergers - a very useful set of idealized simulations

1.5.1.Collisionless mergers

1.5.2.Mergers with gas

1.5.3.Caveats of the merger hypothesis

1.6.Ranking and Matching

2.AB INITIO SIMULATIONS OF GALAXY FORMATION

2.1.Star formation and gas cooling

2.2.The formation of disk dominated systems

2.2.1.Current sub-resolution models for feedback from stellar populations

2.3.The formation of bulge dominated systems

2.3.1.Current models for feedback from super-massive black holes

3.THE NEED FOR ACCURATE MODELLING OF THE GALACTIC INTERSTELLAR MEDIUM AND 'FEEDBACK'

3.1.Supernova explosions

3.2.Stellar winds

3.3.Radiation

3.4.Magnetic fields and cosmic rays

3.5.Mechanical and radiative AGN feedback

4.CONCLUSION & OUTLOOK

REFERENCES