Speaker
Description
Magnetic fields permeate the Universe across a wide range of scales and strengths. On galactic scales, they are amplified by turbulent dynamo processes, eventually saturating at dynamically important levels, and are subsequently transported into the circumgalactic medium by galactic winds. In realistic environments, this evolution involves both direct and inverse turbulent cascades, driven by energy injection from supernovae on small scales and extending up to galactic scales.
These processes can be investigated using numerical simulations. In this work, we study the growth of magnetic fields in an idealized isolated Milky Way–like galaxy using the SWIFT astrophysical simulation code with smoothed particle magnetohydrodynamics (SPH-MHD). We assess the reliability of this approach and identify numerical and physical challenges that arise in modeling galactic dynamos.