In the IllustrisTNG model, CGM gas around z=1 galaxies mixes quickly and separates into cold inner and warm-hot outer phases within 500 Myr due to feedback, with kinematic decorrelation over 400 Myr and ion-specific phases lasting different durations.
@doi [ ] 10.1088/0004-637X/719/1/523, http://adsabs.harvard.edu/abs/2010ApJ...719..523K 719
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Geometry of temperature isosurfaces controls the PDF shape in turbulent multi-phase gas, with clumps transitioning to sheets producing broader distributions.
UV background suppresses NEI in galaxy haloes, restoring equilibrium shock thresholds and producing extended absorption columns for OVI, CIV, and HI beyond the virial radius.
citing papers explorer
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The Thermodynamic and Kinematic Evolution of Circumgalactic Gas around $z=1$ in the IllustrisTNG model
In the IllustrisTNG model, CGM gas around z=1 galaxies mixes quickly and separates into cold inner and warm-hot outer phases within 500 Myr due to feedback, with kinematic decorrelation over 400 Myr and ion-specific phases lasting different durations.
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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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Non-Equilibrium Ionisation in Photoionised Haloes: Implications for Shock Stability and Absorption-Line Signatures
UV background suppresses NEI in galaxy haloes, restoring equilibrium shock thresholds and producing extended absorption columns for OVI, CIV, and HI beyond the virial radius.