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Absorption-line measurements of the circumgalactic medium (CGM) display ahighly non-uniform distribution of lower ionization state species accompaniedby more widespread higher ionization state material. This suggests that the CGMis a dynamic, multiphase medium, such as arises in the presence of turbulence.To better understand this evolution, we perform hydrodynamic andmagneto-hydrodynamic (MHD) simulations of the CGM surrounding Milky Way-likegalaxies. In both cases, the CGM is initially in hydrostatic balance in a$10^{12}$ solar masses dark matter gravitational potential, and the simulationsinclude rotation in the inner halo and turbulence that decreases radially. Theyalso track ionizations, recombinations, and species-by-species radiativecooling in the presence of the redshift-zero UV background, employing theMAIHEM non-equilibrium chemistry package. We find that after 9 Gyrs ofevolution, the presence of a magnetic field leads to an overall hotter CGM,with cool gas in the center where magnetic pressure dominates. While thenon-MHD run produces more cold clouds overall, we find similar Si IV/O VI and NV/O VI ratios between the MHD and non-MHD runs, which are both very differentfrom their equilibrium values. The non-MHD halo develops cool, low angularmomentum filaments above the central disk, in comparison to the MHD run thathas more efficient angular momentum transport, especially for the cold gaswhich forms a more ordered and extended disk late into its evolution.

Modeling Photoionized Turbulent Material in the Circumgalactic Medium III: Effects of Co-rotation and Magnetic Fields