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 redistributing gas in galaxies, depositing metals in the circumgalactic medium, and quenching star formation. The interplay between these outflows and ram-pressure stripping (RPS) due to the galaxy's motion thr...

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Bibliographic Details
Published in:The Astrophysical journal 2018-08, Vol.863 (1), p.49
Main Authors: Bustard, Chad, Pardy, Stephen A., D'Onghia, Elena, Zweibel, Ellen G., Gallagher, J. S.
Format: Article
Language:English
Subjects:
Astrophysics
Computer simulation
Disk galaxies
Fountains
Galactic evolution
Galactic winds
Galaxies
galaxies: dwarf
galaxies: evolution
galaxies: starburst
Magellanic Clouds
Milky Way
Outflow
Ram pressure
Star & galaxy formation
Star formation
Stars & galaxies
Stellar winds
Supernova
Supernovae
Wind models
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Summary:Galactic winds and fountains driven by supernova-heated gas play an integral role in redistributing gas in galaxies, depositing metals in the circumgalactic medium, and quenching star formation. The interplay between these outflows and ram-pressure stripping (RPS) 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 RPS 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 H i 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.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aad08f