EDP Sciences
Free Access
Issue
A&A
Volume 464, Number 1, March II 2007
Page(s) 143 - 154
Section Cosmology (including clusters of galaxies)
DOI https://doi.org/10.1051/0004-6361:20066427
Published online 19 December 2006


A&A 464, 143-154 (2007)
DOI: 10.1051/0004-6361:20066427

Buoyant bubbles in a cooling intracluster medium

I. Hydrodynamic bubbles
A. Gardini1, 0, 2

1  Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL, 61801, USA
    e-mail: gardini@astro.uiuc.edu
2  National Center for Supercomputing Applications, Urbana, IL, 61801, USA

(Received 21 September 2006 / Accepted 9 November 2006)

Abstract
Aims.Over the past several years, numerous examples of X-ray cavities coincident with radio sources have been observed in so-called "cool core" clusters of galaxies. Motivated by these observations, we explore the evolution and the effect of cavities on a cooling intracluster medium (ICM) numerically, adding relevant physics step by step.
Methods.In this paper we present a first set of hydrodynamical, high resolution (10243 effective grid elements), three-dimensional simulations, together with two-dimensional test cases. The simulations follow the evolution of radio cavities, modeled as bubbles filled by relativistic plasma, in the cluster atmosphere, while the ICM is subject to cooling.
Results.We find that the bubble rise retards the development of a cooling flow by inducing motions in the ICM, which repeatedly displace the material in the core. Even bubbles initially set significantly far from the cluster center affect the cooling flow, although much later than the beginning of the simulation. The effect is, however, modest: the cooling time is increased by at most only 25%. As expected, the overall evolution of pure hydrodynamic bubbles is at odds with observations, showing that some additional physics has to be considered to match the data.


Key words: galaxies: clusters: general -- cooling flows -- methods: numerical



© ESO 2007

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