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X-ray Cavities and Cooling Flows

Published online by Cambridge University Press:  30 March 2016

Paul E. J. Nulsen ,
Brian R. McNamara ,
Laurence P. David  and
Michael W. Wise
Paul E. J. Nulsen
Affiliation:
School of Engineering Physics, University of Wollongong, Wollongong NSW 2522, Australia, and Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA
Brian R. McNamara
Affiliation:
Department of Physics and Astronomy, Ohio University, Athens, OH 45701, USA
Laurence P. David
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA
Michael W. Wise
Affiliation:
Massachusetts Institute of Technology, Center for Space Research, 70 Vassar St, Building 37, Cambridge, MA 02139, USA

Abstract

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Recent data have radically altered the X-ray perspective on cooling flow clusters. X-ray spectra show that very little of the hot intra-cluster medium is cooler than about 1 keV, despite having short cooling times. In an increasing number of cooling flow clusters, the lobes of a central radio source are found to have created cavities in the hot gas. Generally, the cavities are not overpressured relative to the intra-cluster gas, but act as buoyant bubbles of radio emitting plasma that drive circulation as they rise, mixing and heating the intra-cluster gas. All this points to the radio source, i.e., an active galactic nucleus, as the heat source that prevents gas from cooling to low temperatures. However, heating due to bubbles alone seems to be insufficient, so the energetics of cooling flows remain obscure. We briefly review the data and theory supporting this view and discuss the energetics of cooling flows.

Type
I. Joint Discussions
Information
Highlights of Astronomy , Volume 13 , 2005 , pp. 307 - 311
Copyright
Copyright © Astronomical Society of Pacific 2005

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