HST narrow-band imaging of M82's southern wind reveals a connected network of compact filaments (typical widths ~5.3 pc) whose covering fraction and flux contribution decline with height, while line ratios indicate photoionization near the disk transitioning to increasing shock heating in the diffus
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The resolution independence of cooling rates in TRML simulations is an artifact of opposing numerical effects with no physical basis, and phase structure converges only when the turbulent Field length (where eddy turnover time equals cooling time) is resolved.
JWST observations find constant ~1% PAH abundance in the M82 superwind to 5 kpc, consistent with shielding in surface layers of cool clouds and possible replenishment.
citing papers explorer
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The Small-scale Structures in the Wind of Messier 82
HST narrow-band imaging of M82's southern wind reveals a connected network of compact filaments (typical widths ~5.3 pc) whose covering fraction and flux contribution decline with height, while line ratios indicate photoionization near the disk transitioning to increasing shock heating in the diffus
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Ceci n'est pas une Couche de M\'elange: The Meaning of Resolved Turbulent Radiative Mixing
The resolution independence of cooling rates in TRML simulations is an artifact of opposing numerical effects with no physical basis, and phase structure converges only when the turbulent Field length (where eddy turnover time equals cooling time) is resolved.
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JWST Observations of Starbursts: Dust Processing in the M82 Superwind
JWST observations find constant ~1% PAH abundance in the M82 superwind to 5 kpc, consistent with shielding in surface layers of cool clouds and possible replenishment.