Bubbles in planetary nebulae and clusters of galaxies: instabilities at bubble’ fronts

Soker, Noam

doi:10.1016/j.newast.2003.12.003

Cited by 2 publications

(5 citation statements)

References 23 publications

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“…Rather, the primary role of turbulence is to improve the mixing of the thermal energy from the interior of the heated cavities into the surrounding cold gas (e.g. Soker 2004;Sternberg et al 2007). This means that while in the run, the bubbles deposit most of their internal energy at the resolution-dependent radius at which they get disrupted, as indicated by the spike in temperature at R ≈ 30 kpc.…”

Section: Periodic Bubblesmentioning

confidence: 99%

“…Comparing this value to the turbulent kinetic energy in our simulations, we find that E turb is only %1% of this overall energy; thus, we do not expect the energy of the turbulent motions themselves to play a major role in the heating of the cool-core region in the ICM. Rather, the key impact of turbulence is to increase the efficiency with which the thermal energy of the rising cloud is mixed into its surroundings (e.g., Soker 2004;Sternberg et al 2007;Sternberg & Soker 2008b). In this sense it behaves much more like heat conduction (e.g., Narayan & Medvedev 2001;Voigt & Fabian 2004;Ruszkowski et al 2004;Sternberg et al 2007) than an energy source.…”

mentioning

confidence: 99%

“…As suggested by the singlebubble runs, and as quantified for the 5DCER run below, these differences are not due to additional energy input from dissipated turbulent kinetic energy. Rather, the primary role of turbulence is to improve the mixing of the thermal energy from the interior of the heated cavities into the surrounding cold gas (e.g., Soker 2004;Sternberg et al 2007). This means that while in the pure hydro run, the bubbles deposit most of their internal energy at the resolution-dependent radius at which they get disrupted, as indicated by the spike in temperature at R % 30 kpc.…”

mentioning

confidence: 99%

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Subgrid Modeling of AGN‐driven Turbulence in Galaxy Clusters

Scannapieco

Brüggen

2008

Astrophysical Journal

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Hot, underdense bubbles powered by active galactic nuclei (AGNs) are likely to play a key role in halting catastrophic cooling in the centers of cool-core galaxy clusters. We present three-dimensional simulations that capture the evolution of such bubbles, using an adaptive mesh hydrodynamic code, FLASH3, to which we have added a subgrid model of turbulence and mixing. While pure hydro simulations indicate that AGN bubbles are disrupted into resolution-dependent pockets of underdense gas, proper modeling of subgrid turbulence indicates that this is a poor approximation to a turbulent cascade that continues far beyond the resolution limit. Instead, Rayleigh-Taylor instabilities act to effectively mix the heated region with its surroundings, while at the same time preserving it as a coherent structure, consistent with observations. Thus, bubbles are transformed into hot clouds of mixed material as they move outward in the hydrostatic intracluster medium (ICM), much as large airbursts lead to a distinctive ''mushroom cloud'' structure as they rise in the hydrostatic atmosphere of Earth. Properly capturing the evolution of such clouds has important implications for many ICM properties. In particular, it significantly changes the impact of AGNs on the distribution of entropy and metals in cool-core clusters such as Perseus.

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Section: Periodic Bubblesmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Subgrid Modeling of AGN‐driven Turbulence in Galaxy Clusters

Scannapieco

Brüggen

2008

Astrophysical Journal

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“…Paper 3 (Soker 2004b). Paper 3 studies the stability of off‐centre low‐density fat bubbles in clusters of galaxies and in PNs to the Rayleigh–Taylor instability.…”

Section: Introductionmentioning

confidence: 99%

“…It was found that to inflate fat, more or less spherical, bubbles the opening angle of the jets should be large; the half opening angle measured from the symmetry axis of each jet should typically be α 40 • , or the jets might precess. Paper-3 (Soker 2004b). Paper 3 studies the stability of off-center low-density fat bubbles in clusters of galaxies and in PNs to the Rayleigh-Taylor instability.…”

Section: Introductionmentioning

confidence: 99%

Bubbles in planetary nebulae and clusters of galaxies: jet bending

Soker

Bisker

2006

Monthly Notices of the Royal Astronomical Society

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We study the bending of jets in binary stellar systems. A compact companion accretes mass from the slow wind of the mass‐losing primary star, forms an accretion disc and blows two opposite jets. These fast jets are bent by the slow wind. Disregarding the orbital motion, we find the dependence of the bending angle on the properties of the slow wind and the jets. Bending of jets is observed in planetary nebulae which are thought to be the descendants of interacting binary stars. For example, in some of these planetary nebulae, the two bubbles (lobes) which are inflated by the two opposite jets are displaced to the same side of the symmetry axis of the nebula. Similar displacements are observed in bubble pairs in the centre of some clusters and groups of galaxies. We compare the bending of jets in binary stellar systems with that in clusters of galaxies.

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Bubbles in planetary nebulae and clusters of galaxies: instabilities at bubble’ fronts

Cited by 2 publications

References 23 publications

Subgrid Modeling of AGN‐driven Turbulence in Galaxy Clusters

Subgrid Modeling of AGN‐driven Turbulence in Galaxy Clusters

Bubbles in planetary nebulae and clusters of galaxies: jet bending

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