We describe a new method that only focuses on the local region surrounding an infalling dwarf in an effort to understand how the hot baryonic halo alters 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 to have survived 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 a dwarf in isolation , but only if the dwarf retains gas for a sufficiently long period of time .
In addition , dwarfs that formed substantial numbers of stars post-infall have a slightly elevated [ Mg / Fe ] at high metallicity ( [ Fe / H ] \sim -1.5 ) .