The aim of the proposed thesis is to investigate the underlying gas physics of the process of gas accretion both through detailed gas modeling and in comparison with observations. How and what fraction of the infalling gas is ultimate accreted onto the galaxy proper is strongly dependent on how the gravitational energy is dissipated and the range of evolutionary paths which determines the physical and chemical state the gas.

We propose an original approach to this problem with combines simulations, ISM microphysics, and observations. This unique and novel program will provide strong constraints on the gas physics that is at the heart of the accretion of gas onto galaxies. The student will learn how to use his work to adapt large-scale cosmological simulations of galaxy formation and evolution.