The Co-Evolution of a Magnetized Intracluster Medium and Hot Galactic
  Coronae: Magnetic Field Amplification and Turbulence Generation
  We use adaptive-mesh magnetohydrodynamic simulations to study the effect of
magnetic fields on ram pressure stripping of galaxies in the intracluster
medium (ICM). Although the magnetic pressure in typical clusters is not strong
enough to affect the gas mass loss rate from galaxies, magnetic fields can
affect the morphology of stripped galaxies. ICM magnetic fields are draped
around orbiting galaxies and aligned with their stripped tails. Magnetic fields
suppress shear instabilities at the galaxy-ICM interface, and magnetized tails
are smoother and narrower than tails in comparable hydrodynamic simulations in
Vijayaraghavan & Ricker (2015). Orbiting galaxies stretch and amplify ICM
magnetic fields, amplifying magnetic power spectra on $10 - 100$ kpc scales.
Galaxies inject turbulent kinetic energy into the ICM via their turbulent wakes
and $g$-waves. The magnetic energy and kinetic energy in the ICM increase up to
$1.5 - 2$ Gyr of evolution, after which galaxies are stripped of most of their
gas, and do not have sufficiently large gaseous cross sections to further
amplify magnetic fields and inject turbulent kinetic energy. The increase in
turbulent pressure due to galaxy stripping and generation of $g$-waves results
in an increase in the turbulent volume fraction of the ICM. This turbulent
kinetic energy is not a significant contributor to the overall ICM energy
budget, but greatly impacts the evolution of the ICM magnetic field.
Additionally, the effect of galaxies on magnetic fields can potentially be
observed in high resolution Faraday rotation measure (RM) maps as small scale
fluctuations in the RM structure.
