The post-infall evolution of a satellite galaxy
  As galaxy simulations increase in resolution more attention is being paid
towards the evolution of dwarf galaxies and how the simulations compare to
observations. Despite this increasing resolution we are however, far away from
resolving the interactions of satellite dwarf galaxies and the hot coronae
which surround host galaxies. We describe a new method which focuses only on
the local region surrounding an infalling dwarf in an effort to understand how
the hot baryonic halo will alter the chemodynamical evolution of dwarf
galaxies. Using this method we examine how a dwarf, similar to Sextans dwarf
spheroidal, evolves in the corona of a Milky Way like galaxy. We find that even
at high perigalacticons the synergistic interaction between ram pressure and
tidal forces transform a dwarf into a stream, suggesting that Sextans was much
more massive in the past in order survive its perigalacticon passage. In
addition the large confining pressure of the hot corona allows gas that was
originally at the outskirts to begin forming stars, initially forming stars of
low metallicity compared to the dwarf evolved in isolation. This increase in
star formation eventually allows a dwarf galaxy to form more metal rich stars
compared to one in isolation, but only if the dwarf retains gas for a
sufficiently long period of time. In addition, dwarfs which formed substantial
numbers of stars post-infall will have a slightly elevated [Mg/Fe] at high
metallicity ([Fe/H] -1.5).
