  One process affecting gas-rich cluster galaxies is ram pressure stripping,
i.e. the removal of galactic gas through direct interaction with the
intracluster medium. Galactic magnetic fields may have an important impact on
the stripping rate and tail structure. We run the first magnetohydrodynamic
simulations of ram pressure stripping that include a galactic magnetic field,
using 159 pc resolution throughout our entire domain in order to resolve mixing
throughout the tail. We find very little difference in the total amount of gas
removed from the unmagnetized and magnetized galaxies, although a magnetic
field with a radial component will initially accelerate stripped gas more
quickly. In general, we find that magnetic fields in the disk lead to slower
velocities in the stripped gas near the disk and faster velocities farther from
the disk. We also find that magnetic fields in the galactic gas lead to larger
unmixed structures in the tail. Finally, we discuss whether ram pressure
stripped tails can magnetize the ICM. We find that the total magnetic energy
density grows as the tail lengthens, likely through turbulence. There are
microGauss-strength fields in the tail in all of our MHD runs, which survive to
at least 100 kpc from the disk (the edge of our simulated region), indicating
that the area-filling factor of magnetized tails in a cluster could be large.
