Chemodynamics of dwarf galaxies under ram-pressure
  By implementing a dynamic wind-tunnel model in a smoothed-particle
chemodynamic/hydrodynamic simulation suite, we have investigated the effects of
ram pressure and tidal forces on dwarf galaxies similar to the Magellanic
Clouds, within host galaxies with gas and dark matter halos that are varied, to
compare the relative effects of tides and ram pressure. We concentrate on how
the distributions of metals are affected by interactions. We find that while
ram pressure and tidal forces have some effect on dwarf galaxy outflows, these
effects do not produce large differences in the metal distributions of the
dwarf disks other than truncation in the outer regions in some cases, and that
confinement from the host galaxy gas halo appears to be more significant than
ram pressure stripping. We find that stochastic variations in the star
formation rate can explain the remaining variations in disk metal properties.
This raises questions on the cause of low metallicities in dwarf galaxies.
