Speaker
Description
Mediated by magnetic field fluctuations, cosmic rays give and take energy from the thermal gas. That energy conversion depends on how cosmic rays are transported. As the local Alfven speed changes, their transport can switch between diffusion, streaming, and advection. Because of the change in density and magnetic field strength between the galactic disk and the galactic halo, there could be a switch from diffusion to streaming or advection between the disk and halo. This shift in cosmic ray transport would impact the outflow of gas from the disk, possibly reducing a galactic wind to a fountain flow. Using CR+MHD simulations, we examine the impact of cosmic rays on the disk-halo interface, focusing on how a change in cosmic-ray transport between the galactic disk and the halo can change the dynamics of gas at the interface. This work is an extension of the study in our recent preprint (https://arxiv.org/abs/2412.12249).
