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We present a hydrodynamical simulation of the turbulent, magnetized,supernova (SN)-driven interstellar medium (ISM) in a stratified box thatdynamically couples the injection and evolution of cosmic rays (CRs) and aself-consistent evolution of the chemical composition. CRs are treated as arelativistic fluid in the advection-diffusion approximation. The thermodynamicevolution of the gas is computed using a chemical network that follows theabundances of H+, H, H2, CO, C+, and free electrons and includes(self-)shielding of the gas and dust. We find that CRs perceptibly thicken thedisk with the heights of 90% (70%) enclosed mass reaching ~1.5 kpc (~0.2 kpc).The simulations indicate that CRs alone can launch and sustain strong outflowsof atomic and ionized gas with mass loading factors of order unity, even insolar neighborhood conditions and with a CR energy injection per SN of 10^50erg, 10% of the fiducial thermal energy of an SN. The CR-driven outflows havemoderate launching velocities close to the midplane (~100 km/s) and are denser(\rho~1e-24 - 1e-26 g/cm^3), smoother, and colder than the (thermal) SN-drivenwinds. The simulations support the importance of CRs for setting the verticalstructure of the disk as well as the driving of winds.

Launching cosmic-ray-driven outflows from the magnetized interstellar medium