The aim of this book is to study the role of interstellar turbulence in the process of star formation. We demonstrate that supersonic turbulent motions significantly affect various properties of the interstellar medium. Therefore, we run numerical simulations of molecular clouds in different environments. In particular, we study typical clouds located in the Milky Way disk as well as clouds which can be found in more extreme regions in our Galaxy, e. g. in the Central Molecular Zone near the Galactic Center.
