Cosmological simulations represent the most complete approach to investigate the complex interplay among the physical processes that shape the evolution of the Universe. In my talk, I will highlight the tremendous progress made in this field by introducing a set of calculations with explicitly include a self-consistent treatment for the evolution of magnetic fields. The simulations are performed with a state of the art cosmological simulations featuring a cutting-edge, moving-mesh treatment for (magneto-)hydrodynamics. I will mainly focus on the properties of magnetic fields in these simulations, and how they are affected by the inclusion of baryon physics processes that are thought to be relevant for galaxy formation. In particular, I will show that the simulations are able to capture the amplification of tiny seed fields present in the early Universe to the B field values observed nowadays in galaxy and galaxy clusters. I will also discuss the potential effects of varying the magnetic seed field intensity on the properties of the simulated galaxy population. Finally, I will describe current developments on the future generation of cosmological MHD simulations.
Coffee: 2:30 pm, 241 Compton