Galaxies are pivotal cosmic laboratories for a wide range of phenomena, from determining the chemical enrichment of the universe — essential for life — to testing the limits of fundamental physics through the refinement of dark matter and dark energy models. Developing a comprehensive theory of galaxy evolution is exceptionally challenging due to the vast range of interconnected scales involved. Microphysical phenomena, such as the interplay between magnetic fields and cosmic rays on sub-au scales, spark large-scale processes that qualitatively transform galactic halos, hundreds of kiloparsecs from the stellar disk. These global galactic properties, in turn, dictate the conditions that govern the behavior and stability of astrophysical plasmas within the interstellar and circumgalactic media (ISM, CGM). Directly simulating or observing all relevant galactic processes is currently infeasible, as the relevant range of physical scales easily exceeds ten orders of magnitude. Therefore, advancing galaxy models requires innovative approaches that combine theoretical insights with observational tests. In this talk, I will highlight my recent work, which uses this combined approach to constrain the role of cosmic rays in shaping the CGM. I will then discuss how upcoming technological advancements will unlock progress for a variety of astrophysical topics.