MHD simulations show CNM clouds are elongated along the local magnetic field with lower disorder per column density than the WNM, explaining the f_CNM-polarization trend for low-cloud-count sightlines.
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astro-ph.GA 2years
2026 2verdicts
UNVERDICTED 2representative citing papers
3D wind-tunnel simulations in the χ~10^3 regime show clump-cocoon geometry sets SB_X/SB_Hα~3, with Hα fraction fixed by atomic physics and X-ray fraction set by residence time in the X-ray band that scales inversely with pressure.
citing papers explorer
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Phase-dependent magnetic coherence in the turbulent interstellar medium
MHD simulations show CNM clouds are elongated along the local magnetic field with lower disorder per column density than the WNM, explaining the f_CNM-polarization trend for low-cloud-count sightlines.
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Clumps in a Cocoon: Geometry and Mixing Set the Universal X-ray to H$\alpha$ Surface Brightness Ratio
3D wind-tunnel simulations in the χ~10^3 regime show clump-cocoon geometry sets SB_X/SB_Hα~3, with Hα fraction fixed by atomic physics and X-ray fraction set by residence time in the X-ray band that scales inversely with pressure.