AGN Heating through Cavities and Shocks

P. E. J. Nulsen; C. Jones; W. R. Forman; L. P. David; B. R. McNamara; D. A. Rafferty; L. Birzan; M. W. Wise

doi:10.1007/978-3-540-73484-0_37

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arXiv · astro-ph/0611136

AGN Heating through Cavities and Shocks

P. E. J. Nulsen·C. Jones·W. R. Forman·L. P. David·B. R. McNamara·D. A. Rafferty·L. Birzan·M. W. Wise

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Abstract

Three comments are made on AGN heating of cooling flows. A simple physical argument is used to show that the enthalpy of a buoyant radio lobe is converted to heat in its wake. Thus, a significant part of ``cavity'' enthalpy is likely to end up as heat. Second, the properties of the repeated weak shocks in M87 are used to argue that they can plausibly prevent gas close to the AGN from cooling. As the most significant heating mechanism at work closest to the AGN, shock heating probably plays a critical role in the feedback mechanism. Third, results are presented from a survey of AGN heating rates in nearby giant elliptical galaxies. With inactive systems included, the overall AGN heating rate is reasonably well matched to the total cooling rate for the sample. Thus, intermittent AGN outbursts are energetically capable of preventing the hot atmospheres of these galaxies from cooling and forming stars.

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P. E. J. Nulsen, C. Jones, W. R. Forman, L. P. David, B. R. McNamara, D. A. Rafferty, L. Birzan, M. W. Wise. 2006-11-04. AGN Heating through Cavities and Shocks. https://doi.org/10.1007/978-3-540-73484-0_37

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