Numerical studies of the interstellar medium on galactic scales
05 / 1998 - 03 / 2005
We propose an investigation of the nature, role and importance of the physical processes involved in the formation and merger-driven evolution of galaxies, using an SPH code. The novelty of our approach consists of the accurate treatment of interstellar matter physics. The formation and evolution of stars is included in a semi-empirical manner, and feedback from supernova explosions is included as well. The code has been demonstrated to work well on isolated and merging galaxies, automatically producing a realistic multiphase interstellar medium and a Schmidt-type star formation law. For the project proposed here the code will be adapted to include extreme parameters appropiate for the high-z universe (e.g. cooling without metals). This programme will allow us to assess the importance of dissipation, feedback and initial conditions on galaxy formation, and the role that major mergers play in the subsequent evolution of galaxies. Expected results include bias between dark and luminous matter, origin of the segregation of molecular and atomic gas, fate of tidally expelled gas, formation of tidal dwarfs, properties and fate of the central molecular component.