Impact of magnetic fields on ram pressure stripping in disk galaxies
  (abridged) Ram pressure can remove significant amounts of gas from galaxies
in clusters, and thus has a large impact on the evolution of cluster galaxies.
Recent observations have shown that key properties of ram pressure stripped
tails of galaxies are in conflict with predictions by simulations. To increase
the realism of existing simulations, we simulated for the first time a disk
galaxy exposed to a uniformly magnetized wind including radiative cooling and
self-gravity of the gas. We find that B-fields have a strong effect on the
morphology of the gas in the tail of the galaxy. While in the pure hydro case
the tail is very clumpy, the MHD case shows very filamentary structures in the
tail. The filaments can be strongly supported by magnetic pressure and, when
this is the case, the B-field vectors tend to be aligned with the filaments.
The ram pressure stripping may lead to the formation of magnetized density
tails that appear as bifurcated in the plane of the sky and resemble the double
tails observed in ESO 137-001 and ESO 137-002. Such tails can be formed under a
variety of situations, both for the disks oriented face-on with respect to the
ICM wind and for the tilted ones. While this bifurcation is due to the generic
tendency for the B-fields to produce very filamentary tail morphology, the tail
properties are further shaped by the combination of the B-field orientation and
the sliding of the field past the disk surface exposed to the wind. Magnetic
draping does not strongly change the rate of gas stripping. For a face-on
galaxy, the field tends to reduce the amount of stripping compared to the pure
hydro case, and is associated with the formation of a magnetic draping layer on
the side of the galaxy exposed to the ICM wind. For significantly tilted disks,
the stripping rate may be enhanced by the ``scraping'' of the disk surface by
the B-fields sliding past the ISM/ICM interface.
