Speaker
Description
In previous work, we have shown that magnetic fields are fundamental to the evolution of MW-like galaxies. Specifically, in the Auriga model, magnetohydrodynamic (MHD) simulations produce realistic galaxies with spiral arm structure and radially-extended discs, whilst their hydrodynamic counterparts are systematically smaller, and exhibit bar and stellar ring features not observed in nature. In this talk, I will show how magnetic fields produce this difference by modifying the transport of angular momentum. This has myriad effects including: the suppression of bar instabilities, the re-shaping of star formation sites, and an increased growth of the central black hole. Together, these effects act to switch the dominant channel of feedback from stellar- to active galactic nuclei (AGN)-driven. In turn, this substantially impacts the evolution of the circumgalactic medium (CGM). In the last part of my talk, I will discuss the applicability of our results to other galaxy formation models, and explain why our results cannot be replicated by the tuning of feedback models alone.
