outburst event (see @veilleux_etal05 for a review). Star formation can drive outflows through a combination of stellar winds from young stars and multiple type-II supernova explosions [e.g., @leitherer_etal99], while black hole accretion episodes can produce energetic jets or winds that inflate a cavity with thermal and non-thermal particles [e.g., @mcnamara_nulsen07; @yuan_narayan14]. Both of these scenarios are critical events in galaxy evolution, as they both can deposit significant amounts of energy into the rest of the galaxy on scales $\gtrsim$10 kpc (see @mcnamara_nulsen07 for a review). However, the details of these “feedback” effects (mass displacement, energy transport, etc.) are poorly understood since we observe them in external galaxies. The Fermi bubbles are a unique laboratory for understanding these processes since we can spatially resolve the bubbles across multiple wavebands.

A popular strategy to probe these effects and bubbles’ origins has been the use of magnetohydrodynamic (MHD) simulations to reproduce the bubbles’ global morphology and non-thermal properties. Simulations produce cosmic rays either from a black hole accretion event [@zubovas_etal11; @guo_mathews12a; @guo_mathews12b; @yang_etal12; @yang_etal13; @zubovas_nayakshin12; @mou_etal14; @mou_etal15], from nuclear star formation activity [@crocker12; @crocker_etal14; @crocker_etal15; @sarkar_etal15; @ruszkowski_etal16], or in-situ as the bubbles evolve [@cheng_etal11; @cheng_etal15b; @mertsch_sarkar11; @fujita_etal14; @lacki14; @sasaki_etal15], and compare the non-thermal 