How Magnetic Fields Regulate Cooling and Mixing in Turbulent Radiative Mixing Layers

arXiv:2609.29782 · astro-ph.GA · Submitted 2026-09-24 · Read on arXiv

astro-ph.GA

Submitted: 2026-09-24

Updated: 2026-09-24

Code: https://github.com/IAS-Astrophysics/athenak

Terminology

• Anisotropy — 3× in this paper · explained in 3 episodes
• Core — 2× in this paper · explained in 2 episodes
• Velocity Dispersion — 2× in this paper · explained in 2 episodes
• Alignment — 1× in this paper · explained in 1 episode
• Benchmark — 1× in this paper · explained in 2 episodes
• Entrainment — 1× in this paper · explained in 2 episodes
• Magnetohydrodynamics (MHD) — 1× in this paper · explained in 3 episodes

Sources

• Clumps in a Cocoon: Geometry and Mixing Set the Universal X-ray to H$\alpha$ Surface Brightness Ratio
• Array Programming with NumPy
• Ceci n'est pas une Couche de M'elange: The Meaning of Resolved Turbulent Radiative Mixing
• The Origin of Da Scaling: Suppressed Cooling in Fast-Cooling Mixing Layers
• Magnetised CGM Gas at z~1 revealed by SPICE-RACS
• Multiphase gas in Circumgalactic cloud complexes: Insights from kiloparsec-scale Magnetohydrodynamic Turbulence Simulations
• Universal Structure of Turbulent Radiative Mixing Layers
• A universal correlation between warm and hot gas in the stripped tails of cluster galaxies

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