MHD simulations of ram pressure stripping of a disk galaxy
  The removal of the interstellar medium (ISM) of disk galaxies through ram
pressure stripping (RPS) has been extensively studied in numerous simulations.
Nevertheless, the role of magnetic fields (MF) on the gas dynamics in this
process has been hardly studied, although the MF influence on the large-scale
disk structure is well established. With this in mind, we present a 3D
magnetohydrodynamic (MHD) simulation of face-on RPS of a disk galaxy to study
the impact of the galactic MF in the gas stripping. The main effect of
including a galactic MF is a flared disk. When the intracluster medium (ICM)
wind hits this flared disk, oblique shocks are produced at the interaction
interface, where the ISM is compressed, generating a gas inflow from large
radii towards the central regions of the galaxy. This inflow is observed for
$\sim 150$ Myr and may supply the central parts of the galaxy with material for
star formation while the outskirts of the disk are being stripped of gas, thus
the oblique shocks can induce and enhance the star formation in the remaining
disk. We also observed that the MF alters the shape and structure of the swept
gas, giving a smooth appearance in the magnetized case and clumpier and
filamentary-like morphology in the hydro case. Finally, we estimated the
truncation radius expected for our models using the Gunn-Gott criterion and
found that is in agreement with the simulations.
