SN explosions, stellar winds, spiral arms and galaxy mergers are among the most important astrophysical phenomena responsible for the galaxy evolution at different scales and for the continue production of shock waves and turbulence in the interstellar medium (ISM) and intergalactic medium (IGM). Recently, both observational and numerical work have begun to suggest that these supersonic turbulent flows may be controlling the molecular clouds formation, the initial mass distribution of stars and the process of star formation. Depending on the conditions of the environment where these phenomena take place and on the amount of injected energy, gas outflows (galactic winds and galactic fountains) may also develop, changing the mass content of the galaxies and spreading metals and turbulence over large scales. Here, we aim to investigate all these processes at the different scales, from pc to kpc, employing both analytical and a numerical modeling for a global understanding of the galaxy evolution and the consequent processes of clouds and stars formation, their initial mass function, and the typical conditions under which an environment (at any scale) may be subject to a high star formation rate (starburst regions) or not.
News published in Agência FAPESP Newsletter about the scholarship: