Cluster Heating by Viscous Dissipation of Sound Waves

By M. Ruszkowski, M. Brüggen, M. Begelman. 2003

160 citations recorded by the source corpus.

We simulate the effects of viscous dissipation of waves that are generated by active galactic nucleus (AGN) activity in clusters of galaxies. We demonstrate that the amount of viscous heating associated with the dissipation of these waves can offset radiative cooling rates in cooling flow clusters of galaxies. This heating mechanism leads to spatially distributed and approximately symmetrical dissipation. The heating waves reach a given distance from the cluster center on a timescale shorter than the cooling time. This means that this heating mechanism has the potential to quench cooling flows in a quasi-stable fashion. Moreover, the heating is gentle, as no strong shocks are present in the simulations. We first investigated whether a single continuous episode of AGN activity can lead to adequate dissipation to balance cooling rates. These simulations demonstrated that whereas secondary waves generated by the interaction of the rising bubble with the intracluster medium are clearly present, viscous heating associated with the dissipation of these waves is insufficient to balance radiative cooling. It is only when the central source is intermittent that the viscous dissipation of waves associated with subsequent episodes of activity can offset cooling. This suggests that the ripples observed in the Perseus Cluster can be interpreted as being due to the AGN duty cycle; i.e., they trace AGN activity history. The simulations were performed using the adaptive mesh refinement code FLASH in two dimensions.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

The relation between accretion rate and jet power in X-ray luminous elliptical galaxies (2006, background): “Some additional energy will also be transfered into sound waves (Churazov et al. 2002; Fabian et al. 2003, 2005, 2006; Forman et al. 2003; Ruszkowski et al. 2004).”
A very deep Chandra observation of the Perseus cluster: shocks, ripples and conduction (2005, background): “Such an energy transportand dissipation mechanism is roughly isotropic and can therebyprovide the required gently distributed heat source required by observation c© 0000 RAS of this and other similarly X-ray peaked clusters (Ruszkowski et al 2004a,b,2005; Reynolds et al 2005; Fabian et al 2005).”
Filaments, Bubbles, and Weak Shocks in the Gaseous Atmosphere of M87 (2006, background): “The energy of jets and buoyant bubbles can be transferred to the radiating gas by shocks, gravity waves, or turbulence (e.g., Churazov et al. 2002; Ruszkowski et al. 2004a, 2004b; Begelman 2004; Omma et al. 2004; Roychowdhury et al. 2004, 2005; Heinz&Churazov 2005;Mathews et al. 2006; Binney et al.…”
The Cluster-Scale AGN Outburst in Hydra A (2004, background): “If, as it is now, the shock was strongest in the regions of lowest preshock pressure, near to the outer lobes, it would have propagated farthest in those regions (as in the simulations of Ruszkowski et al. 2004).”
Heating Hot Atmospheres with Active Galactic Nuclei (2007, background): “In numerical simulations, shocks are controlled by viscous stresses (Ruszkowski et al. 2004a,b; Brüggen et al. 2005), so that these two processes are lumped together.”
A deeper X‐ray study of the core of the Perseus galaxy cluster: the power of sound waves and the distribution of metals and cosmic rays (2007, background): “Such sound waves can transport significant energy in a roughly isotropic manner and so balance radiative cooling of the intracluster gas if they dissipate their energy over the surrounding 50–100 kpc (Fabian et al. 2003a; Ruszkowski et al. 2004; Fabian et al. 2005).”
CAUSE AND EFFECT OF FEEDBACK: MULTIPHASE GAS IN CLUSTER CORES HEATED BY AGN JETS (2011, background): “The coupling may occur, for example, via turbulent mixing of AGN bubbles with the ICM (Scannapieco & Brüggen 2008), viscous dissipation of weak shocks (Ruszkowski et al. 2004a,b), and cosmic ray heating (Guo & Oh 2008; Ruszkowski et al. 2008; Sharma et al. 2009).”
Mechanical feedback from active galactic nuclei in galaxies, groups and clusters (2012, background): “Ruszkowski et al (2004) showed that heating by sound dissipation might also be able to offset cooling in the long term.”
Simulating galaxy formation with black hole driven thermal and kinetic feedback (2016, methodology): “…taken, often using bipolar outflows in idealized simulations of hydrostatic haloes (Reynolds et al. 2002; Basson & Alexander 2003; Omma et al. 2004; Ruszkowski et al. 2004; Zanni et al. 2005; Brighenti & Mathews 2006; Brüggen et al. 2007; Cattaneo & Teyssier 2007; Sternberg et al. 2007;…”
X-ray Spectroscopy of Cooling Clusters (2005, methodology): “This is the heating mechanism of the ’effervescent heating’ approach of Begelman (2001) (see also Ruszkowski et al. 2004a).”
Reflections of Active Galactic Nucleus Outbursts in the Gaseous Atmosphere of M87 (2003, background): “901 the formation of the 14 kpc ring is similar to that of Ruszkowski et al. (2004), in which impulsive energy injection generates weak shocks as the injected energy forms a cocoon in the galaxy atmosphere in the Virgo core.”
What is a cool-core cluster? a detailed analysis of the cores of the X-ray flux-limited HIFLUGCS cluster sample (2009, background): “…(e.g. Zakamska & Narayan 2003), central AGN heating via direct cosmic ray-ICM interaction+conduction (Guo & Oh 2008), AGN heating by bubble induced weak shocks (e.g. Mathews et al. 2006), soundwaves+conduction (e.g. Ruszkowski et al. 2004) and turbulence+ onduction (e.g. Dennis & Chandran 2005).”
Feedback heating by cosmic rays in clusters of galaxies (2007, methodology): “Numerical simulations of AGN bubbles (and jets, in some cases) in the ICM have been performed by a number of authors (e.g. Brüggen & Kaiser 2002; Ruszkowski et al. 2004; Vernaleo & Reynolds 2006; Reynolds et al. 2005).”
Galaxy formation theory (2010, background): “…al. 2004; Vecchia et al. 2004; Ruszkowski et al. 2008, but see Vernaleo and Reynolds 2006) to heating by outflows drivenby super-Eddington accretion (King 2009) and viscous dissipation of sound waves (Ruszkowski et al. 2004) with turbulence playing an important role (Brüggen and Scannapieco 2009).”