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Cosmic rays (CRs) are an important component in the interstellar medium(ISM), but their effect on the dynamics of the disk-halo interface (< 10 kpcfrom the disk) is still unclear. We study the influence of CRs on the gas abovethe disk with high-resolution FIRE-2 cosmological simulations of late-typeLstar galaxies at redshift around zero. We compare runs with and without CRfeedback (with constant anisotropic diffusion around 3e29 cm^2/s andstreaming). Our simulations capture the relevant disk halo interactions,including outflows, inflows, and galactic fountains. Extra-planar gas in all ofthe runs satisfies dynamical balance, where total pressure balances the weightof the overlying gas. While the kinetic pressure from non-uniform motion(>1-kpc scale) dominates in the midplane, thermal and bulk pressures (or CRpressure if included) take over at large heights. We find that with CRfeedback, (1) the warm (1e4K) gas is slowly accelerated by CRs; (2) the hot (>5e5K) gas scale height is suppressed; (3) the warm-hot (2e4-5e5K) mediumbecomes the most volume-filling phase in the disk-halo interface. We develop anovel conceptual model of the near-disk gas dynamics in low-redshift Lstargalaxies: With CRs, the disk-halo interface is filled with CR-driven warm windsand hot super-bubbles that are propagating into the CGM with a small fractionfalling back to the disk. Without CRs, most outflows from hot superbubbles aretrapped by the existing hot halo and gravity, so typically they form galacticfountains.

The impact of cosmic rays on dynamical balance and disk-halo interaction in Lstar disk galaxies