Simulation of radio plasma in clusters of galaxies
Corresponding Author
M. Brüggen
1 MPI für Astrophysik, Karl-Schwarzschild-Strasse 1, 85740 Garching, Germany
2 International University Bremen, Campus Ring 1, 28759 Bremen, Germany
3 Churchill College, Storey's Way, Cambridge CB3 0DS
[email protected]Search for more papers by this authorC. R. Kaiser
4 Department of Physics & Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ
Search for more papers by this authorE. Churazov
1 MPI für Astrophysik, Karl-Schwarzschild-Strasse 1, 85740 Garching, Germany
5 Space Research Institute (IKI), Profsouznaya 84/32, Moscow 117810, Russia
Search for more papers by this authorT. A. Enßlin
1 MPI für Astrophysik, Karl-Schwarzschild-Strasse 1, 85740 Garching, Germany
Search for more papers by this authorCorresponding Author
M. Brüggen
1 MPI für Astrophysik, Karl-Schwarzschild-Strasse 1, 85740 Garching, Germany
2 International University Bremen, Campus Ring 1, 28759 Bremen, Germany
3 Churchill College, Storey's Way, Cambridge CB3 0DS
[email protected]Search for more papers by this authorC. R. Kaiser
4 Department of Physics & Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ
Search for more papers by this authorE. Churazov
1 MPI für Astrophysik, Karl-Schwarzschild-Strasse 1, 85740 Garching, Germany
5 Space Research Institute (IKI), Profsouznaya 84/32, Moscow 117810, Russia
Search for more papers by this authorT. A. Enßlin
1 MPI für Astrophysik, Karl-Schwarzschild-Strasse 1, 85740 Garching, Germany
Search for more papers by this author1 Available at http://www.jb.man.ac.uk/atlas/
Abstract
We present three-dimensional hydrodynamical simulations of buoyant gas in a typical cluster environment. In these simulations, hot matter was injected continuously into a small region offset from the cluster centre. In agreement with previous analytic estimates, we found that the bubbles evolve very differently depending on the rate of energy injection. Using tracer particles we computed the efficiency of the bubbles to stir the intracluster medium (ICM) and find that recurrent low-power sources are more effective in mixing the inner cluster region than rarer large outbursts. Moreover, we computed radio maps of the bubbles based on different assumptions about the magnetic field. In the radio band the bubbles closely resemble FR I sources. For the bubbles to be detectable for long enough to account for FR I sources, we found that reacceleration has to take place. The bubbles are generally difficult to detect, both in the radio and in the X-ray band. Thus it is possible to hide a significant amount of energy in the form of bubbles in clusters.
Acknowledgments
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Some of the computations reported here were performed using the UK Astrophysical Fluids Facility (UKAFF). This work was supported by the European Community Research and Training Network ‘The Physics of the Intergalactic Medium’. We thank W. Forman for many useful comments. MB also acknowledges support through a Junior Research Fellowship from Churchill College and thanks Jim Pringle for helpful discussions.
Acknowledgments
This paper has been typeset from a tex/latex file prepared by the author.
