Bubbles, feedback and the intracluster medium: three-dimensional hydrodynamic simulations

By Vicent Quilis, Richard G. Bower, M. Balogh. 2001

137 citations recorded by the source corpus.

We use a three-dimensional hydrodynamical code to simulate the effect of energy injection on cooling flows in the intracluster medium. Specifically, we compare a simulation of a 1015-M⊙ cluster with radiative cooling only with a second simulation in which thermal energy is injected 31 kpc off-centre, over 64 kpc3 at a rate of for 50 Myr. The heat injection forms a hot, low-density bubble which quickly rises, dragging behind it material from the cluster core. The rising bubble pushes with it a shell of gas which expands and cools. We find the appearance of the bubble in X-ray temperature and luminosity to be in good qualitative agreement with recent Chandra observations of cluster cores. Toward the end of the simulation, at 600 Myr, the displaced gas begins to fall back toward the core, and the subsequent turbulence is very efficient at mixing the low- and high-entropy gas. The result is that the cooling flow is disrupted for up to ∼ 50 Myr after the injection of energy ceases. Thus this mechanism provides a very efficient method for regulating cooling flows, if the injection events occur with a 1:1 duty cycle.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/cd96938e5c12210aa2eaae3286153f26861a0298

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Citations in the corpus

Filaments, Bubbles, and Weak Shocks in the Gaseous Atmosphere of M87 (2006, background): “These bubbles can be a significant energy source for the cooling gas and can explain much of the radio and X-ray morphology (Churazov et al. 2001, 2002; Quilis et al. 2001; Brüggen et al. 2002).”
A unified model for AGN feedback in cosmological simulations of structure formation (2007, background): “There has been considerable effort from the theoretical point of view (e.g. Binney & Tabor, 1995; Churazov et al., 2001, 2002; Quilis et al., 2001; Ruszkowski & Begelman, 2002; Dalla Vecchia et al., 2004; Kawata & Gibson, 2005; Sijacki & Springel, 2006; Thacker et al., 2006; Okamoto et al., 2007)…”
Spatially resolved X-ray spectroscopy of cooling clusters of galaxies (2003, unknown): “…gas outwards (Churazov et al. 2001), halo-in-halo structure (Makishima et al. 2001), turbulent mixing due to rising and falling hot gas bubbles (Quilis et al. 2001), heating by AGN activity (Böhringer et al. 2002), contamination due to non-thermal X-ray emission (McCarthy et al. 2002),…”
Heating cooling flows with jets (2003, methodology): “Only the simulations of Quilis et al. (2001) and Brüggen et al. (2002) are fully threedimensional, and only Brüggen & Kaiser (2002) had an adaptive grid; unfortunately, this two-dimensional simulation had slab rather than rotational symmetry.”
Breaking the hierarchy of galaxy formation (2005, background): “…idea that has gained popularity in recent years is that energy injected from AGN in the form of radio jets is responsible for switching off cooling at the centre of massive haloes (Quilis et al. 2001; Bruggen & Kaiser 2002; Churazov et al. 2002; Dalla Vecchia et al. 2004; Sijacki & Springel 2006).”
X-ray Spectroscopy of Cooling Clusters (2005, methodology): “Many groups have now carried out numerical hydrodynamical simulations of the behaviour of bubbles in the ICM (Brüggen & Kaiser 2001; Quilis et al. 2001; Brüggen & Kaiser 2002; Brüggen 2003; Basson & Alexander 2003; Omma & Binney 2004; Omma et al. 2004; Ruszkowski & Begelman 2002; Ruszkowski et…”
Heating Hot Atmospheres with Active Galactic Nuclei (2007, background): “As well as providing better models for the convection associated with anisotropic cavity heating, 3D simulations allow more realistic treatments of cavity stability and mixing (Quilis et al. 2001).”
Hot Gas In and Around Elliptical Galaxies (2003, background): “Quilis et al. (2001) studied the evolution of a nearly axisymmetric 3D bubble produced by heated gas at some finite radius, simulating jet heating.”
Cluster Heating by Viscous Dissipation of Sound Waves (2003, background): “…models in which the mechanical energy supply to the cluster is momentum driven (e.g., Tabor & Binney (1993); Reynolds et al. (2001)) and those in which it is buoyancy driven (e.g., Churazov et al. (2001); Brüggen et al. (2002); Brüggen & Kaiser (2002); Brüggen (2003); Quilis et al. (2001)).”
Hydrodynamical simulations of cluster formation with central AGN heating (2005, methodology): “In particular, for galaxy clusters of similar masses as considered by Quilis et al. (2001) and Dalla Vecchia et al. (2004), and with bubbles parametrized in an analogous way, we find that the changes in gas properties induced by AGN heating, e.g. density and temperature radial profiles and central…”
What Shapes the Luminosity Function of Galaxies? (2003, background): “It must therefore punch a well-collimated hole through the halo or remain contained within a buoyant bubble that is convected out of the halo (Quilis et al. 2001; Springel &Hernquist 2003; Kay et al. 2002).”
High-Resolution X-Ray Spectroscopic Constraints on Cooling-Flow Models for Clusters of Galaxies (2002, background): “—Time-dependent AGN outflow heating models have been considered by a variety of authors (e.g., Rosner & Tucker 1989; Tabor & Binney 1993; Binney & Tabor 1995; Churazov et al. 2001; Brüggen & Kaiser 2001; Quilis et al. 2001; David et al. 2001; Nulsen et al. 2002; Kaiser & Binney 2003).”