SILCC VII -- Gas kinematics and multiphase outflows of the simulated ISM at high gas surface densities

Abstract

We present magnetohydrodynamic (MHD) simulations of the star-forming multiphase interstellar medium (ISM) in stratified galactic patches with gas surface densities ${\Sigma }_{\mathrm{gas}}=$ 10, 30, 50, and 100 ${\mathrm{M}}_{\odot }\mathrm{p}{\mathrm{c}}^{-2}$. The SILCC project simulation framework accounts for non-equilibrium thermal and chemical processes in the warm and cold ISM. The sink-based star formation and feedback model includes stellar winds, hydrogen-ionising UV radiation, core-collapse supernovae, and cosmic ray (CR) injection and diffusion. The simulations follow the observed relation between ${\Sigma }_{\mathrm{gas}}$ and the star formation rate surface density ${\Sigma }_{\mathrm{SFR}}$. CRs qualitatively change the outflow phase structure. Without CRs, the outflows transition from a two-phase (warm and hot at 1 kpc) to a single-phase (hot at 2 kpc) structure. With CRs, the outflow always has three phases (cold, warm, and hot), dominated in mass by the warm phase. The impact of CRs on mass loading decreases for higher ${\Sigma }_{\mathrm{gas}}$ and the mass loading factors of the CR-supported outflows are of order unity independent of ${\Sigma }_{\mathrm{SFR}}$. Similar to observations, vertical velocity dispersions of the warm ionised medium (WIM) and the cold neutral medium (CNM) correlate with the star formation rate as ${\sigma }_{\mathrm{z}}\propto {\Sigma }_{\mathrm{SFR}}^a$, with $a\sim 0.20$. In the absence of stellar feedback, we find no correlation. The velocity dispersion of the WIM is a factor $\sim 2.2$ higher than that of the CNM, in agreement with local observations. For ${\Sigma }_{\mathrm{SFR}}\gtrsim 1.5\times 10^{-2}{\mathrm{M}}_{\odot }{\mathrm{yr}}^{-1}{\mathrm{kpc}}^{-2}$ the WIM motions become supersonic.

20 pages, 12 figures, accepted by MNRAS

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