# Cosmic Ray Driven Outflows from the Large Magellanic Cloud: Contributions to the LMC Filament

**Authors:** Chad Bustard, Ellen G. Zweibel, Elena D'Onghia, J. S. Gallagher III, Ryan Farber  
**arXiv:** [1911.02021](https://arxiv.org/abs/1911.02021)  
**Date:** 2019-11-05  
**Summary page:** https://www.summarizepaper.com/en/paper/1911.02021v2/

## Key points

- Simulations of magnetized cosmic ray driven outflows from the Large Magellanic Cloud (LMC) were conducted
- LMC's star formation history was used to seed outflow generation
- Different LMC gas masses and cosmic ray transport treatments were explored
- Findings suggest that much of the outflow-turned-halo gas is shielded on the far-side of the LMC due to its primarily face-on infall through the Milky Way halo over the past Gyr
- On its near-side, past outflows have fought an uphill battle against ram pressure resulting in a smaller halo mass compared to its far-side
- Absorption line studies probing only LMC foreground may severely underestimate total mass of LMC halo formed by outflows
- Clustered stellar feedback is an important factor in shaping galactic winds
- Valuable insights into recent magnetized cosmic ray driven outflows from LMC and their contributions to filament formation are provided.

## Summary

This paper presents simulations of recent magnetized cosmic ray driven outflows from the Large Magellanic Cloud (LMC), incorporating the LMC's star formation history to seed outflow generation. The simulations explore different LMC gas masses and cosmic ray transport treatments, with comparisons made to published outflow flux estimates, neutral and ionized hydrogen observations, and Faraday rotation measure maps. Additionally, the study reports on the gas mass that becomes unbound from the LMC disk and swept by ram pressure into the Trailing Magellanic Stream. The findings suggest that even for the largest outburst considered in this study, much of the outflow-turned-halo gas is shielded on the far-side of the LMC due to its primarily face-on infall through the Milky Way halo over the past Gyr. On its near-side however, past outflows have fought an uphill battle against ram pressure resulting in a halo mass at least a factor of a few smaller than that on its far-side. The authors note that absorption line studies probing only LMC foreground may severely underestimate total mass of LMC halo formed by outflows. This paper also highlights clustered stellar feedback as an important factor in shaping galactic winds and suggests further exploration of this aspect in future studies. Overall, this paper provides valuable insights into recent magnetized cosmic ray driven outflows from LMC and their contributions to filament formation while emphasizing important considerations for future observational studies.