The majority of galactic baryons reside outside of the galactic disk in the diffuse gas known as the circumgalactic medium (CGM). While state-of-the art simulations excel at reproducing galactic disk properties, many struggle to drive strong galactic winds or to match the observed multiphase structure of the CGM with thermal supernova feedback. To remedy this, recent studies have included non-thermal cosmic ray (CR) stellar feedback prescriptions to drive strong outflows and to better match observed low-ion column densities in the CGM. However promising, these results depend strongly on the choice of CR transport mechanism and its constant parameter values, thus weakening the predictive power of such simulations. Using a suite of simulated isolated disk galaxies, I will demonstrate that the invoked approximation of CR transport affects the predicted temperature and ionization structure of the CGM.
