Evolution of Buoyant Bubbles in M87

By E. Churazov, M. Brüggen, C. Kaiser, H. Böhringer, W. Forman. 2000

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The morphology of the X-ray- and radio-emitting features in the central ~50 kpc region around the galaxy M87 strongly suggests that buoyant bubbles of cosmic rays (inflated by an earlier nuclear active phase of the galaxy) rise through the cooling gas at roughly half the sound speed. In the absence of strong surface tension, initially spherical bubbles will transform into tori as they rise through an external medium. Such structures can be identified in the radio images of the halo of M87. During their rise, bubbles will uplift relatively cool X-ray-emitting gas from the central regions of the cooling flow to larger distances. This gas is colder than the ambient gas and has a higher volume emissivity. As a result, rising "radio" bubbles may be trailed by elongated X-ray features, as indeed is observed in M87. We performed simple hydrodynamic simulations to illustrate qualitatively the evolution of buoyant bubbles in the M87 environment.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/4235338be4a63d2670863c95eb48dc8b65227bf8

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Citations in the corpus

Feedback heating by cosmic rays in clusters of galaxies (2007, background): “…& Narayan 2003; Voigt & Fabian 2004) or turbulent mixing (Kim & Narayan 2003b; Dennis & Chandran 2005) and heating by outflows, bubbles or sound waves from a central active galactic nuclei (e.g., Churazov et al. 2001; Brüggen & Kaiser 2002; Ruszkowski & Begelman 2002; Ruszkowski et al. 2004).”
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).”
Accretion onto the Supermassive Black Hole in M87 (2002, methodology): “More often, it seems that jets are responsible for inflating bubbles in the surrounding ISM, which then expand buoyantly (i.e., roughly at the sound speed; Churazov et al. 2001; Reynolds, Heinz, & Begelman 2002) and give rise to radio lobes and corresponding X-ray structures.”
Investigating AGN heating in a sample of nearby clusters (2006, methodology): “…we have used the buoyancy time-scale (tage = tb = R/vb) as these are expected to be rising buoyantly up through the ICM, with the buoyancy velocity given by vb = √ 2gV SCD , (3) where CD = 0.75 is the drag coefficient (Churazov et al. 2001) and S = πr2w is the cross-sectional area of the bubble.”
X-Ray Emission from the Hot Interstellar Medium and Southwest Radio Lobe of the Nearby Radio Galaxy Centaurus A (2003, background): “Since the launch of Chandra, many additional examples of the interactions between the ICM and the jets of radio galaxies have been detected (Churazov et al. 2001; Finoguenov & Jones 2001; McNamara et al. 2000; David et al. 2001; Fabian et al. 2000; Blanton et al. 2001b).”
Spatially resolved X-ray spectroscopy of cooling clusters of galaxies (2003, unknown): “Worked-out examples include metallicity inhomogeneities (Fabian et al. 2001), buoyantly rising radio bubbles transporting cool 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),…”
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)…”
XMM—Newton observations of the Perseus cluster — II. Evidence for gas motions in the core (2003, background): “On the other hand, activity of the supermassive black hole can induce turbulence on a smaller scales through the mechanical action of the outflows (Churazov et al. 2001,2002, Reynolds, Heinz & Begelman 2002, Brüggen & Kaiser 2002).”
On the Nature of Feedback Heating in Cooling Flow Clusters (2004, methodology): “For C we shall adopt the value C ≃ 0.75 used by Kaiser (2003) and derived from the numerical simulations by Churazov et al. (2001).”
Cooling flows as a calorimeter of active galactic nucleus mechanical power (2002, methodology): “In the discussion below, we present a qualitative picture based particularly on the ROSAT, Chandra and XMM-Newton data on M87 and NGC 1275 (Böhringer et al. 1993, 1995, 2001a, 2001b, Fabian et al. 2000, Churazov et al., 2000, 2001).”
Mechanical feedback from active galactic nuclei in galaxies, groups and clusters (2012, background): “Uplift of low entropy gas with rising cavities and the fallback that is likely to follow (Churazov et al 2001, Gitti et al 2011) and flow around buoyant bubbles can also generate turbulence in the ICM (Sanders et al 2011).”
A deep Chandra observation of the Perseus cluster: shocks and ripples (2003, background): “The process is due not to effervescence of many small bubbles (Begelman 2001), to rare major eruptions (Soker et al. 2001; Kaiser & Binney 2002) or to the buoyant bubbles themselves (Churazov et al. 2001), but to a more continuous dissipation of acoustic energy as the (attached) bubbles grow.”
On the prevalence of radio‐loud active galactic nuclei in brightest cluster galaxies: implications for AGN heating of cooling flows (2006, result): “Hydrodynamic simulations have been able to reproduce bubbles with properties similar to those observed (e.g. Churazov et al. 2001; Quilis, Bower & Balogh 2001; Brüggen & Kaiser 2002; Brüggen 2003) and have also shown that, provided that radio source activity is recurrent, the total energy…”
Discovery of Ghost Cavities in the X-Ray Atmosphere of Abell 2597 (2001, unknown): “Since the cavities have a lower gas density than their surroundings, they should behave like bubbles in water and rise buoyantly in the intracluster medium (ICM; McNamara et al. 2000b; Churazov et al. 2001).”
Cluster Heating by Viscous Dissipation of Sound Waves (2003, background): “This means that, depending on the effective value of γ (which can range between 4/3 and 5/3), 25 − 40% of the energy input can be transferred to the ambient medium (see also, e.g., Churazov et al. 2001).”
The Blast Wave Model for AGN Feedback: Effects on AGN Obscuration (2008, background): “Buoyant bubbles (see Reynolds et al. 2001; Churazov et al. 2001) and expanding blast waves (see Cavaliere et al. 2002; Lapi et al. 2005) constitute viable mechanisms for such a transport.”
Gas entropy in a representative sample of nearby X-ray galaxy clusters (REXCESS): relationship to gas mass fraction (2009, background): “If this were indeed the case, it would imply that AGN heating is achieved via mechanisms such as weak shocks (e.g., Fabian et al. 2003), or buoyant bubbles (e.g., Churazov et al. 2001), rather than via catastrophic explosions.”
Heating Hot Atmospheres with Active Galactic Nuclei (2007, background): “This results in the formation of a vortex ring around the cavity after it has been overrun (Churazov et al. 2001; Enßlin & Brüggen 2002).”
AGN Feedback and Cooling Flows: Problems with Simple Hydrodynamic Models (2005, background): “More recent numerical investigations have explored the buoyant evolution of the cocoon after its supersonic expansion phase (Churazov et al. 2001; Brüggen & Kaiser 2001, 2002; Reynolds et al. 2002; Basson & Alexander 2003; Omma et al. 2004; Omma & Binney 2004; Dalla Vecchia et al. 2004; Robinson…”