Key points are not available for this paper at this time.
Despite being energetically important, the effect of cosmic rays on the dynamics of the interstellar medium (ISM) is assumed to be negligible because the cosmic ray energy diffusion coefficient parallel to the magnetic field is relatively large. Using numerical simulations, we explore how variation of the cosmic ray diffusion coefficient as a function of gas temperature could impact the dynamics of the ISM. We create a two-zone model of cosmic ray transport, reflecting the strong damping of the small scale magnetic field fluctuations, which scatter the cosmic rays, in a gas with low ionization. The variable diffusion coefficient allows more cold gas to form. However, setting the diffusion coefficient at a critical value in the warm phase allows the cosmic rays to adjust the kinetic energy cascade. Specifically, we show the slope of the cascade changes for motion perpendicular to the mean magnetic field, whereas kinetic energy parallel to the magnetic field is reduced equally across inertial scales. We show that cosmic ray energization (or reacceleration) comes at the expense of total radiated energy generated during the formation of a cold cloud. We also show that our two-zone model of cosmic ray transport is capable of matching estimates of the grammage for some paths through the simulation, but full comparison of the grammage requires simulating turbulence in a larger volume.
Habegger et al. (Tue,) studied this question.