Title: Dynamical impact of cosmic rays in the interstellar medium

Abstract: Cosmic rays (CRs) are an important component in the interstellar medium with comparable energy densities to the kinetic and thermal ones. As such, they constitute a large energy reservoir with unique properties. Contrary to the thermal energy, the bulk of the CRs cool very inefficiently. In addition, they are not directly coupled to the gas but can diffuse or stream relative to the gas. These two properties allow CRs to escape from their acceleration sites (mostly supernova remnants), populate large fractions of the volume of the galaxy and are able to deposit energy and momentum at far distances from the typically violent regions of star formation and stellar feedback. Using numerical simulations, I will illustrate how CR are able to drive strong galactic outflows with different properties compared to the thermally driven counterparts. I will discuss the important parameters in CR transport that determine the dynamical impact in the interstellar medium. I will also show a new class of CR simulations, in which we couple spectrally resolved CRs with more accurate cooling and energy dependent transport to the magneto-hydrodynamic simulations.