Heating cooling flows with jets

Omma, Henrik; Binney, James; Bryan, Greg L.; Slyz, Adrianne

doi:10.1111/j.1365-2966.2004.07382.x

Cited by 223 publications

(276 citation statements)

References 82 publications

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“…When the jets penetrate to too large distances no fat bubbles are formed, while in intermediate cases elongated bubbles and/or bubbles detached from the center are formed (e.g., Basson & Alexander 2003;Omma et al 2004;Heinz et al 2006;Vernaleo & Reynolds 2006;Alouani Bibi et al 2007;O'Neill & Jones 2010;Mendygral et al 2011Mendygral et al , 2012.…”

Section: The Jetsmentioning

confidence: 99%

“…Another one is the structure of many small-scale vortices that develop inside the bubble and in the ICM in the vicinity of the bubble. Vortices play important roles in entrainment of gas by the jets and bubbles (e.g., Omma et al 2004;Gilkis & Soker 2012), in the stability of bubbles (see below), and most important in the mixing of hot bubble gas with the ICM. This mixing is a most important process, as it might be the main heating process of the ICM (as discussed in section 4.3).…”

Section: Jet-inflated Bubblesmentioning

confidence: 99%

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The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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I review the influence jets and the bubbles they inflate might have on their ambient gas as they operate through a negative jet feedback mechanism (JFM). I discuss astrophysical systems where jets are observed to influence the ambient gas, in many cases by inflating large, hot, and low-density bubbles, and systems where the operation of the JFM is still a theoretical suggestion. The first group includes cooling flows in galaxies and clusters of galaxies, star-forming galaxies, young stellar objects, and bipolar planetary nebulae. The second group includes core collapse supernovae, the common envelope evolution, the grazing envelope evolution, and intermediate luminosity optical transients. The suggestion that the JFM operates in these four types of systems is based on the assumption that jets are much more common than what is inferred from objects where they are directly observed. Common to all eight types of systems reviewed here is the presence of a compact object inside an extended ambient gas. The ambient gas serves as a potential reservoir of mass to be accreted on to the compact object. If the compact object launches jets as it accretes mass, the jets might reduce the accretion rate as they deposit energy to the ambient gas, or even remove the entire ambient gas, hence closing a negative feedback cycle.

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Section: The Jetsmentioning

confidence: 99%

Section: Jet-inflated Bubblesmentioning

confidence: 99%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

View full text Add to dashboard Cite

show abstract

“…Omma et al 2004;Heinz & Churazov 2005;Roediger et al 2007;Sternberg & Soker 2008b;Gilkis & Soker 2012). Some cool regions further cool and flow inward to feed the AGN.…”

Section: Introductionmentioning

confidence: 99%

Heating the intracluster medium by jet-inflated bubbles

Hillel

Soker

2015

Mon. Not. R. Astron. Soc.

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We examine the heating of the intra-cluster medium (ICM) of cooling flow clusters of galaxies by jet-inflated bubbles and conclude that mixing of hot bubble gas with the ICM is more important than turbulent heating and shock heating. We use the pluto hydrodynamical code in full 3D to properly account for the inflation of the bubbles and to the multiple vortices induced by the jets and bubbles. The vortices mix some hot shocked jet gas with the ICM. For the parameters used by us the mixing process accounts for about four times as much heating as that by the kinetic energy in the ICM, namely, turbulence and sound waves. We conclude that turbulent heating plays a smaller role than mixing. Heating by shocks is even less efficient.

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“…The initial rapid expansion of the bubbles may drive shocks that propagate through intracluster medium (ICM) and heat the gas (e.g., Fabian et al 2003;Forman et al 2007; Randall et al 2015;Reynolds, Balbus, & Schekochihin 2015). With time, rapid expansion decelerates and the bubbles continue to grow subsonically until they start rising buoyantly in the cluster atmosphere, uplifting cool gas, exciting gravity waves, and driving turbulence (Churazov et al 2002;Omma et al 2004;. One of the alternative scenarios is that the bubbles themselves are composed of hot thermal plasma and efficiently mix with the ICM heating the gas (Hillel & Soker 2014;Soker, Hillel, & Sternberg 2015).…”

Section: Introductionmentioning

confidence: 99%

The nature and energetics of AGN-driven perturbations in the hot gas in the Perseus Cluster

Zhuravleva

Churazov

Arévalo

et al. 2016

Mon. Not. R. Astron. Soc.

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Cores of relaxed galaxy clusters are often disturbed by AGN. Their Chandra observations revealed a wealth of structures induced by shocks, subsonic gas motions, bubbles of relativistic plasma, etc. In this paper, we determine the nature and energy content of gas fluctuations in the Perseus core by probing statistical properties of emissivity fluctuations imprinted in the soft-and hard-band X-ray images. About 80 per cent of the total variance of perturbations on ∼ 8 − 70 kpc scales in the inner region have an isobaric nature, i.e., are consistent with slow displacements of the gas in pressure equilibrium with ambient medium. Observed variance translates to the ratio of nonthermal to thermal energy of ∼ 13 per cent. In the region dominated by weak "ripples", about half of the total variance is also associated with isobaric perturbations on scales a few tens of kpc. If these isobaric perturbations are induced by buoyantly rising bubbles, then these results suggest that most of the AGN-injected energy should first go into bubbles rather than into shocks. Using simulations of a shock propagating through the Perseus atmosphere, we found that models reproducing the observed features of a central shock have more than 50 per cent of the AGN-injected energy associated with the bubble enthalpy and only about 20 per cent is carried away with the shock. Such energy partition is consistent with the AGN-feedback model, mediated by bubbles of relativistic plasma, and supports the importance of turbulence in the balance between gas heating and radiative cooling.

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Heating cooling flows with jets

Cited by 223 publications

References 82 publications

The jet feedback mechanism (JFM) in stars, galaxies and clusters

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Heating the intracluster medium by jet-inflated bubbles

The nature and energetics of AGN-driven perturbations in the hot gas in the Perseus Cluster

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