Heating cooling flows with jets

By Henrik Omma, J. Binney, Greg BryanAdrianne Slyz. 2003

194 citations recorded by the source corpus.

Active galactic nuclei are clearly heating gas in ‘cooling flows’. The effectiveness and spatial distribution of the heating are controversial. We use three-dimensional simulations on adaptive grids to study the impact on a cooling flow of weak, subrelativistic jets. The simulations show cavities and vortex rings as in the observations. The cavities are fast-expanding dynamical objects rather than buoyant bubbles as previously modelled, but shocks still remain extremely hard to detect with X-rays. At late times the cavities turn into overdensities that strongly excite the g modes of a cluster. These modes damp on a long time-scale. Radial mixing is shown to be an important phenomenon, but the jets weaken the metallicity gradient only very near the centre. The central entropy density is modestly increased by the jets. We use a novel algorithm to impose the jets on the simulations.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0a37598c27d4ea2b8678f146aeee80e905e38daa

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Citations in the corpus

Nuclear Activity in Nearby Galaxies (2008, background): “…energy from small-scale jets or collimated outflows provides a major source of “feedback” into the circumnuclear environment, perhaps to the extent that accretion can be significantly interrupted or curtailed (Binney & Tabor 1995; Di Matteo et al. 2003; Pellegrini et al. 2003a; Omma et al. 2004).”
Heating Hot Atmospheres with Active Galactic Nuclei (2007, methodology): “AGN-induced mixing has been explored recently by several groups using 2D and 3D hydrodynamical simulations (Brüggen 2002; Omma et al. 2004; Heath et al. 2006; Roediger et al. 2006).”
A semi-analytic model for the co-evolution of galaxies, black holes and active galactic nuclei (2008, background): “…could counteract cooling flows has been discussed for many years (e.g. Binney & Tabor 1995; Churazov et al. 2002; Fabian et al. 2003; Binney 2004; Omma et al. 2004), these observations now make it possible to investigate more quantitatively whether the heating rates are sufficient to offset the…”
The case for AGN feedback in galaxy groups (2009, background): “…et al. 2006, 2008; Croton et al. 2006; Hopkins et al. 2006; Somerville et al. 2008) and suppressing the onset of catastrophic cooling of the hot gas in groups and clusters (e.g,. Churazov et al. 2001; Brighenti & Mathews 2003; Dalla Vecchia et al. 2004; Ruszkowski et al. 2004; Omma et al. 2004).”
Mechanical AGN feedback: controlling the thermodynamical evolution of elliptical galaxies (2012, background): “…et al. 2004; Brüggen, Ruszkowski & Hallman 2005; Mathews & Brighenti 2008; Mathews 2009; Guo & Mathews 2010), or bipolar mechanical outflows/jets (Omma et al. 2004; Soker & Pizzolato 2005; Zanni et al. 2005; Brighenti & Mathews 2006; Vernaleo & Reynolds 2006; Brüggen et al. 2007; Gaspari et…”
Black hole evolution – I. Supernova-regulated black hole growth (2015, background): “…rates on the other hand, the radio mode deposits the AGN feedback energy into a bipolar outflow with a jet velocity of 104 km s−1 into a cylinder with a cross-section of radius x and height 2 x following Omma et al. (2004) (more details about the jet implementation are given in Dubois et al. 2010).”
Jet-regulated cooling catastrophe (2010, methodology): “The choice of the jet velocity input ‖uJ‖ 104 km s−1 (or equivalently the mass loading factor η = 100) is particularly arbitrary but based on earlier work by Omma et al. (2004), Cattaneo & Teyssier (2007) and Dubois et al. (2009).”
On the prevalence of radio‐loud active galactic nuclei in brightest cluster galaxies: implications for AGN heating of cooling flows (2006, background): “Other authors (e.g. Omma et al. 2004; Brighenti & Mathews 2006) have argued that momentum-driven jets are an alternative means of distributing AGN energy throughout the intracluster medium.”
The cosmic evolution of massive black holes in the Horizon-AGN simulation (2016, background): “…on the other hand, the radio mode deposits the AGN feedback energy into a bipolar outflow with a jet velocity of 104 km s−1 into a cylinder with a cross-section of radius x and height 2 x following Omma et al. (2004) (more details about the jet implementation are given in Dubois et al. 2010).”
X-ray Spectroscopy of Cooling Clusters (2005, background): “…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 al. 2004a,b; Robinson et al. 2004; Vecchia et al. 2004; Reynolds 2005).”
The many lives of active galactic nuclei: cooling flows, black holes and the luminosities and colour (2005, background): “A number of authors have suggested ways in which the radio source might replace the thermal energy lost to X-ray emission (Binney & Tabor 1995; Churazov et al. 2002; Brüggen & Kaiser 2002; Ruszkowski & Begelman 2002; Kaiser & Binney 2003; Omma et al. 2004).”
Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters (2009, background): “In particular, a number of studies based on simulations of isolated halos (e.g., Omma et al. 2004; Brighenti & Mathews 2006) have pointed out that gas circulation generated by jets provides an important contribution for the stabilization of cooling flows (see also Heinz et al. 2006, for a…”
Galaxy formation theory (2010, methodology): “For example, Omma et al. (2004) use numerical simulations to show that jets inflate cavities in the hot gas that can excite g modes in the cluster atmosphere and heat the gas, while Roychowdhury et al. (2004) explore a model in which the bubbles are buoyant and heat t atmosphere by doingpdV work as…”
INTRACLUSTER MEDIUM ENTROPY PROFILES FOR A CHANDRA ARCHIVAL SAMPLE OF GALAXY CLUSTERS (2009, background): “…et al. 2001; Churazov et al. 2002; Brüggen & Kaiser 2002; Brüggen et al. 2002; Nath & Roychowdhury 2002; Ruszkowski & Begelman 2002; Alexander 2002; Omma et al. 2004; McCarthy et al. 2004; Roychowdhury et al. 2004; Hoeft & Brüggen 2004; Dalla Vecchia et al. 2004; Soker & Pizzolato 2005;…”
Hot Accretion Flows Around Black Holes (2014, background): “Models that invoke efficient jet heating generally require a relatively slow (sub-relativistic) jet and a mass loss rate in the jet as large as the Eddington rate, which seems unlikely (e.g., Omma et al. 2004).”
Self-regulated growth of supermassive black holes by a dual jet-heating active galactic nucleus feedback mechanism: methods, tests and implications for cosmological simulations (2011, methodology): “Thus, our modelling should be interpreted as a tentative description of the wind arising from a larger region surrounding the BH, and is expected to carry most of the momentum (see Omma et al. 2004 for a more thorough discussion of this issue).”
Radiative Feedback from Massive Black Holes in Elliptical Galaxies: AGN Flaring and Central Starburst Fueled by Recycled Gas (2007, background): “From the numerical point of view, the code is the same as in CO97 and CO01; however, the present simulations are much more difficult to run because the stellar density distribution, being more concentrated than the King model, now injects more gas into the central regions, thus increasing the gas de”
Modelling the galaxy bimodality: shutdown above a critical halo mass (2006, background): “…one possible way for the AGN to heat the gas is through shocks produced by the propagation of jets (e.g. Reynolds et al. 2001; Fabian et al. 2003; Omma et al. 2004), although the problem of how the heat generated by this process is distributed in the hot gas remains open (see also Begelman &…”