Thermal instability produces steady-state temperature fluctuations in the ICM outside cluster cores when conduction is anomalously suppressed by heat-flux-driven instabilities, extending the unstable regime to over half the cluster volume.
@doi [ ] 10.1086/145707, https://ui.adsabs.harvard.edu/abs/1953ApJ...117..431P 117
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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.
Geometry of temperature isosurfaces controls the PDF shape in turbulent multi-phase gas, with clumps transitioning to sheets producing broader distributions.
Low-angular-momentum test-particle models of HVCs originating at tens of kpc in a rotating halo reproduce observed kinematics and imply an accretion rate of several solar masses per year sufficient for long-term star formation.
citing papers explorer
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Latent thermal instability
Thermal instability produces steady-state temperature fluctuations in the ICM outside cluster cores when conduction is anomalously suppressed by heat-flux-driven instabilities, extending the unstable regime to over half the cluster volume.
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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.
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From Clumps to Sheets: Geometry Controls the Temperature PDF of Multi-Phase Gas
Geometry of temperature isosurfaces controls the PDF shape in turbulent multi-phase gas, with clumps transitioning to sheets producing broader distributions.
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Modeling the Accretion of High-Velocity Clouds from a Rotating Halo
Low-angular-momentum test-particle models of HVCs originating at tens of kpc in a rotating halo reproduce observed kinematics and imply an accretion rate of several solar masses per year sufficient for long-term star formation.