The Fate of Supernova-Heated Gas in Star-Forming Regions of the LMC: Lessons for Galaxy Formation

Chad Bustard (Wisconsin-Madison) - October 29, 2018 at 12:10 pm

Abstract: The Magellanic System is an excellent, nearby case-study in galaxy formation and galaxy dynamics. As the Large and Small Magellanic Clouds (LMC and SMC) orbit around each other, they fling material behind them, forming the Trailing Magellanic Stream, an immense reservoir of gas that may someday fall into the Milky Way and enhance our Galactic ecosystem by providing more fuel to form stars. Recent observations suggest that some of this Stream gas may be the relics of past outflows from the Clouds that were swept away by ram pressure, like smoke in a wind. I will present our pilot study of hydrodynamic simulations of ram pressure stripping, supernova-driven outflows, and trailing filament formation behind the LMC. We find that even weak fountain flows, produced by clustered supernovae and solely thermal wind driving, are capable of being expelled from the galaxy due to ram pressure. Preliminary tests of an LMC model with magnetic fields and cosmic ray driven winds are underway. Given our close proximity to the Clouds, we are in a great position to improve our model and constrain it with detailed, multi-wavelength observations, allowing us to test the influences of various small-scale processes on large-scale outflow launching. I’ll present a few ways in which I am exploring the small-scale effects of cosmic rays on their environments and their relevance to large-scale outflow driving.

The seminar will be held in 131A Campbell Hall.

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