Cosmic-Ray Feedback from Supernovae in a Stratified Interstellar Medium (2412.12249v1)

Abstract: Each supernova's energy drives interstellar medium (ISM) turbulence and can help launch galactic winds. What difference does it make if $10\%$ of the energy is initially deposited into cosmic rays? To answer this question and study cosmic-ray feedback, we perform galactic patch simulations of a stratified ISM. We compare two magnetohydrodynamic and cosmic ray (MHD+CR) simulations, which are identical except for how each supernova's energy is injected. In one, $10\%$ of the energy is injected as cosmic-ray energy and the rest is thermal. In the other case, energy injection is strictly thermal. We find that cosmic-ray injections (1) drive a faster vertical motion with more mass, (2) produce a more vertically oriented magnetic field, and (3) increase the scale height of warm gas outside the midplane $(z \gtrsim 0.5\,\mathrm{kpc})$. Both simulations show the formation of cold clouds (with a total mass fraction $>50\%$) through the Parker instability and thermal instability. We also show that the Parker instability leads to a decorrelation of cosmic-ray pressure and gas density. Finally, our simulations show that a vertical magnetic field can lead to a significant decrease in the calorimetric fraction for injected cosmic rays.