The Evolution of Magellanic-like Galaxy Pairs and The Production of
  Magellanic Stream Analogues in Simulations with Tides, Ram Pressure, and
  Stellar Feedback
  We present a series of chemodynamical simulations of Magellanic-like systems
consisting of two interacting, equal-mass dwarf galaxies orbiting a massive
host galaxy, including feedback and star formation, tides, and ram pressure. We
study the star formation and chemical enrichment history of the dwarfs, and the
production of a Magellanic Stream analogue. The dwarfs interact with each other
through tidal forces, distorting their morphologies and triggering star
formation. A stream is naturally produced as outflows, induced by feedback and
interactions, are stretched by tidal forces. Counter to some recent
simulations, we find that the leading arm persists even in the presence of ram
pressure from the host galaxy. Interactions between the dwarfs and the host
galaxies produce multiple kinematic components in the stream, as observed. A
combination of ongoing star-formation and entrained low-metallicity gas causes
the stream to have a complex chemical structure, with an average metallicity
that is generally lower than that of the dwarfs.
