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Non-Kolmogorov turbulence in multiphase intracluster medium driven by cold gas precipitation and AGN jets
Astrophysics of Galaxies · Submitted 21 Dec 2020
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim In the MHD case, turbulence may thus be driven by a combination of AGN jet stirring and filament motions.
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The abstract, sentence by sentence
AGN feedback is responsible for maintaining plasma in global thermal balance in extended halos of elliptical galaxies and galaxy clusters. Local thermal instability in the hot gas leads to the formation of precipitating cold gas clouds that feed the central supermassive black holes, thus heating the hot gas and maintaining global thermal equilibrium. We perform three dimensional MHD simulations of self-regulated AGN feedback in a Perseus-like galaxy cluster with the aim of understanding the impact of the feedback physics on the turbulence properties of the hot and cold phases of the ICM. We find that, in general, the cold phase velocity structure function (VSF) is steeper than the prediction from Kolmogorov's theory. We attribute the physical origin of the steeper slope of the cold phase VSF to the driving of turbulent motions primarily by the gravitational acceleration acting on the ballistic clouds. We demonstrate that, in the pure hydrodynamical case, the precipitating cold filaments may be the dominant agent driving turbulence in the hot ICM. The arguments in favor of this hypothesis are that: (i) the cold phase mass dominates over hot gas mass in the inner cool core; (ii) hot and cold gas velocities are spatially correlated; (iii) both the cold and hot phase velocity distributions are radially biased. We show that, in the MHD case, the turbulence in the ambient hot medium (excluding the jet cone regions) can also be driven by the AGN jets. The driving is then facilitated by enhanced coupling due to magnetic fields of the ambient gas and the AGN jets. In the MHD case, turbulence may thus be driven by a combination of AGN jet stirring and filament motions. We conclude that future observations, including those from high spatial and spectral resolution X-ray missions, may help to constrain self-regulated AGN feedback by quantifying the multi-temperature VSF in the ICM.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | AGN feedback is responsible for maintaining plasma in global thermal balance in extended halos of elliptical galaxies and galaxy clusters. | background 1.00 | 0.04 | 0.04 | asserted 1.00 |
| s1 | Local thermal instability in the hot gas leads to the formation of precipitating cold gas clouds that feed the central supermassive black holes, thus heating the hot gas and maintaining global thermal equilibrium. | background 1.00 | 0.07 | 0.04 | asserted 1.00 |
| s2 | We perform three dimensional MHD simulations of self-regulated AGN feedback in a Perseus-like galaxy cluster with the aim of understanding the impact of the feedback physics on the turbulence properties of the hot and cold phases of the ICM. | method 0.65 | 0.96 | 0.03 | asserted 0.72 |
| s3 | We find that, in general, the cold phase velocity structure function (VSF) is steeper than the prediction from Kolmogorov's theory. | result 1.00 | 0.97 | 0.25 | asserted 1.00 |
| s4 | We attribute the physical origin of the steeper slope of the cold phase VSF to the driving of turbulent motions primarily by the gravitational acceleration acting on the ballistic clouds. | interpretation 1.00 | 0.87 | 0.16 | asserted 0.99 |
| s5 | We demonstrate that, in the pure hydrodynamical case, the precipitating cold filaments may be the dominant agent driving turbulence in the hot ICM. | result 0.95 | 0.92 | 0.15 | hedged possibility 0.60 |
| s6 | The arguments in favor of this hypothesis are that: (i) the cold phase mass dominates over hot gas mass in the inner cool core; (ii) hot and cold gas velocities are spatially correlated; (iii) both the cold and hot phase velocity distributions are radially biased. | interpretation 0.84 | 0.79 | 0.06 | asserted 0.65 |
| s7 | We show that, in the MHD case, the turbulence in the ambient hot medium (excluding the jet cone regions) can also be driven by the AGN jets. | result 0.99 | 0.94 | 0.12 | asserted 0.93 |
| s8 | The driving is then facilitated by enhanced coupling due to magnetic fields of the ambient gas and the AGN jets. | interpretation 0.98 | 0.67 | 0.04 | asserted 0.80 |
| s9 | In the MHD case, turbulence may thus be driven by a combination of AGN jet stirring and filament motions. | interpretation 0.77 | 0.82 | 0.25 | hedged possibility 1.00 |
| s10 | We conclude that future observations, including those from high spatial and spectral resolution X-ray missions, may help to constrain self-regulated AGN feedback by quantifying the multi-temperature VSF in the ICM. | future work 1.00 | 0.11 | 0.44 | hedged possibility 1.00 |
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Original abstract
AGN feedback is responsible for maintaining plasma in global thermal balance in extended halos of elliptical galaxies and galaxy clusters. Local thermal instability in the hot gas leads to the formation of precipitating cold gas clouds that feed the central supermassive black holes, thus heating the hot gas and maintaining global thermal equilibrium. We perform three dimensional MHD simulations of self-regulated AGN feedback in a Perseus-like galaxy cluster with the aim of understanding the impact of the feedback physics on the turbulence properties of the hot and cold phases of the ICM. We find that, in general, the cold phase velocity structure function (VSF) is steeper than the prediction from Kolmogorov's theory. We attribute the physical origin of the steeper slope of the cold phase VSF to the driving of turbulent motions primarily by the gravitational acceleration acting on the ballistic clouds. We demonstrate that, in the pure hydrodynamical case, the precipitating cold filaments may be the dominant agent driving turbulence in the hot ICM. The arguments in favor of this hypothesis are that: (i) the cold phase mass dominates over hot gas mass in the inner cool core; (ii) hot and cold gas velocities are spatially correlated; (iii) both the cold and hot phase velocity distributions are radially biased. We show that, in the MHD case, the turbulence in the ambient hot medium (excluding the jet cone regions) can also be driven by the AGN jets. The driving is then facilitated by enhanced coupling due to magnetic fields of the ambient gas and the AGN jets. In the MHD case, turbulence may thus be driven by a combination of AGN jet stirring and filament motions. We conclude that future observations, including those from high spatial and spectral resolution X-ray missions, may help to constrain self-regulated AGN feedback by quantifying the multi-temperature VSF in the ICM.
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2 arXiv papers cite this in 6 sentences
Papers citing it · 5 sentences without a confident label
Cites it as support 1 paper
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Recent MHD simulations show that efficient coupling, facilitated by magnetic fields, can promote angular momentum transfer between hot gas stirred by jets and cold material, which along with the effects of magnetic braking can have a critical impact on cold gas angular momentum [ref] .
Recent Progress in Modeling the Macro- and Micro-Physics of Radio Jet Feedback in Galaxy Clusters · The Lobe-ICM Interaction · 0.96
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