The Fate of Supernova-Heated Gas in Star-Forming Regions of the LMC:
  Lessons for Galaxy Formation?
  Galactic winds and fountains driven by supernova-heated gas play an integral
role in re-distributing gas in galaxies, depositing metals in the
circumgalactic medium (CGM), and quenching star formation. The interplay
between these outflows and ram pressure stripping due to the galaxy's motion
through an ambient medium may enhance these effects by converting fountain
flows into expelled gas. In this paper, we present controlled, 3D simulations
of ram pressure stripping combined with thermally driven, local outflows from
clustered supernovae in an isolated disk galaxy modeled on the Large Magellanic
Cloud (LMC), a dwarf satellite of the Milky Way on its first infall.
Observational evidence of local outflows emanating from supergiant shells in
the LMC and a trailing filament of HI gas originating from these regions - with
no obvious Leading Arm counterpart - may represent a perfect example of this
process. Our simulations present a proof-of-concept that ram pressure can
convert fountain flows into expelled gas. We find that fountains launched near
the peak star formation time of the LMC can comprise part of the LMC filament
in the Trailing Stream, but with lower column densities than observed. Larger,
more numerous outflows from the LMC may be possible and may contribute more
mass, but higher inertia gas will lengthen the timescale for this gas to be
swept away by ram pressure. Given the high resolution observations, increased
knowledge of star formation histories, and growing evidence of multiphase,
ionized outflows, the LMC is an ideal test-bed for future wind models.
