The authors implement magnetic field-aligned hyperbolic diffusion in SPH and LESPH, showing stability on tests including the magneto-thermal instability where only LESPH with reconstruction allows growth.
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In adiabatically stratified cluster gas the MTI saturates via large plumes destroyed by shear, producing turbulent kinetic energy that scales as χ ω_T.
Presents 24 AREPO+IllustrisTNG zoom-in simulations of clusters above 10^15 solar masses showing converged magnetic fields with volume-averaged plasma beta approximately 100 inside R200 after z~1.2, declining Faraday rotation profiles, and intermittent Braginskii heating approaching cooling rates in
TNG-Cluster simulations find that in galaxy cluster centers turbulence accounts for under half the total velocity dispersion (typically 50-75 km/s), is mostly subsonic, provides sub-percent pressure support, and is primarily driven by SMBH feedback.
50 constrained simulations of Coma cluster analogues reproduce the observed radial X-ray surface brightness and Compton-y profiles within the scatter expected from environment and assembly history.
citing papers explorer
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Fast, Stable, and Physical: Hyperbolic, Magnetic Field-Aligned Diffusion in SPH
The authors implement magnetic field-aligned hyperbolic diffusion in SPH and LESPH, showing stability on tests including the magneto-thermal instability where only LESPH with reconstruction allows growth.
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Magneto-Thermal Instability in Galaxy Clusters -- III. The Limit of Adiabatic Stratification
In adiabatically stratified cluster gas the MTI saturates via large plumes destroyed by shear, producing turbulent kinetic energy that scales as χ ω_T.
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The PICO-Cluster Project: presenting the galaxy cluster sample and studying magnetic field growth, Faraday rotation and Braginskii heating
Presents 24 AREPO+IllustrisTNG zoom-in simulations of clusters above 10^15 solar masses showing converged magnetic fields with volume-averaged plasma beta approximately 100 inside R200 after z~1.2, declining Faraday rotation profiles, and intermittent Braginskii heating approaching cooling rates in
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Bulk vs. turbulent motions at the centres of galaxy clusters: AGN-driven turbulence according to TNG-Cluster
TNG-Cluster simulations find that in galaxy cluster centers turbulence accounts for under half the total velocity dispersion (typically 50-75 km/s), is mostly subsonic, provides sub-percent pressure support, and is primarily driven by SMBH feedback.
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Learning the Universe: Constrained simulations of the Coma galaxy cluster -- I. Radial X-ray and Compton-y signatures
50 constrained simulations of Coma cluster analogues reproduce the observed radial X-ray surface brightness and Compton-y profiles within the scatter expected from environment and assembly history.