Self-regulating AGN jets in MHD simulations of cool-core clusters yield realistic FRI radio morphologies viewed along the jet axis and account for frequency-independent lobe extents via 1-50 μG fields allowing both young and old electrons to radiate.
A., & Sijacki, D
7 Pith papers cite this work, alongside 104 external citations. Polarity classification is still indexing.
7
Pith papers citing it
104
external citations · Pith
abstract
In many observed galaxy clusters, jets launched by the accretion process on to supermassive black holes, inflate large-scale cavities filled with energetic, relativistic plasma. This process is thought to be responsible for regulating cooling losses, thus moderating the inflow of gas on to the central galaxy, quenching further star formation and maintaining the galaxy in a red and dead state. In this paper, we implement a new jet feedback scheme into the moving mesh-code arepo, contrast different jet injection techniques and demonstrate the validity of our implementation by comparing against simple analytical models. We find that jets can significantly affect the intracluster medium (ICM), offset the overcooling through a number of heating mechanisms, as well as drive turbulence, albeit within the jet lobes only. Jet-driven turbulence is, however, a largely ineffective heating source and is unlikely to dominate the ICM heating budget even if the jet lobes efficiently fill the cooling region, as it contains at most only a few per cent of the total injected energy. We instead show that the ICM gas motions, generated by orbiting substructures, while inefficient at heating the ICM, drive large-scale turbulence and when combined with jet feedback, result in line-of-sight velocities and velocity dispersions consistent with the Hitomi observations of the Perseus cluster.
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2026 7verdicts
UNVERDICTED 7representative citing papers
ArkenstoneBH is a new subgrid model for the hot phase of black hole feedback that, in isolated galaxy tests, suppresses star formation by counteracting gas inflows from the circumgalactic medium.
Only the simultaneous presence of AGN jets and winds produces sufficient turbulence via their interaction to suppress star formation in elliptical galaxies; neither component alone is effective.
XRISM measurements indicate turbulent dissipation from jets struggles to balance cooling in cluster atmospheres except possibly in limited inner regions of systems like Hydra A.
MHD simulations indicate that SKA-Mid Band 5a can detect filamentary polarized emission from ICM magnetic fields at high resolution and sensitivity, allowing inference of turbulence driving scales.
Braginskii-MHD simulations of sloshing cluster cores show that pressure-anisotropy limiters plus turbulent magnetic structure reduce effective viscosity far below the Spitzer value, steepening velocity spectra and dissipating a small fraction of turbulent kinetic energy.
Jet and wind feedback from AGN couple nonlinearly through Kelvin-Helmholtz instability, raising energy dissipation efficiency to 0.64 and dropping star formation rate to 10^{-3} solar masses per year.
citing papers explorer
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Simulating realistic radio morphologies of Fanaroff-Riley I jets in a self-regulating cool-core cluster
Self-regulating AGN jets in MHD simulations of cool-core clusters yield realistic FRI radio morphologies viewed along the jet axis and account for frequency-independent lobe extents via 1-50 μG fields allowing both young and old electrons to radiate.
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ArkenstoneBH. A model for high-specific energy black hole feedback in cosmological simulations
ArkenstoneBH is a new subgrid model for the hot phase of black hole feedback that, in isolated galaxy tests, suppresses star formation by counteracting gas inflows from the circumgalactic medium.
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Turbulence and Star Formation Suppression in Elliptical Galaxies: The Role of Active Galactic Nucleus Jet Wind Interaction
Only the simultaneous presence of AGN jets and winds produces sufficient turbulence via their interaction to suppress star formation in elliptical galaxies; neither component alone is effective.
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Are X-ray Atmospheres Heated by Turbulent Dissipation? XRISM Constraints
XRISM measurements indicate turbulent dissipation from jets struggles to balance cooling in cluster atmospheres except possibly in limited inner regions of systems like Hydra A.
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Unraveling the Imprints of Fluctuation-dynamo on the Intracluster Medium with the SKA
MHD simulations indicate that SKA-Mid Band 5a can detect filamentary polarized emission from ICM magnetic fields at high resolution and sensitivity, allowing inference of turbulence driving scales.
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Reduced Effective Viscosity from Anisotropic Transport and Plasma Instabilities in the Sloshing Cores of Galaxy Clusters
Braginskii-MHD simulations of sloshing cluster cores show that pressure-anisotropy limiters plus turbulent magnetic structure reduce effective viscosity far below the Spitzer value, steepening velocity spectra and dissipating a small fraction of turbulent kinetic energy.
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Active Galactic Nucleus Feedback in an Elliptical Galaxy. IV. The Importance of the Jet Wind Coupling
Jet and wind feedback from AGN couple nonlinearly through Kelvin-Helmholtz instability, raising energy dissipation efficiency to 0.64 and dropping star formation rate to 10^{-3} solar masses per year.