New Perspectives on Cooling Flows and Cluster Radio Sources

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dc.creatorMcNamara, B. R.
dc.creatorWise, M. W.
dc.creatorDavid, L. P.
dc.creatorNulsen, P. E. J.
dc.creatorSarazin, C. L.
dc.date2000-12-14
dc.date.accessioned2026-07-07T01:57:02Z
dc.date.available2026-07-07T01:57:02Z
dc.descriptionWe discuss new results from the Chandra X-ray Observatory and XMM-Newton on cluster cooling flows, emphasizing early results from our Chandra programs. We find cooling rates reduced by factors of 5-10 compared to those from earlier missions. Nevertheless, substantial amounts of keV gas appear to be cooling and fueling star formation in central dominant cluster galaxies (CDGs). The structure of the keV thermal gas is remarkably complex, particularly in regions surrounding the the radio source and sites of star formation in CDGs. The radio sources are displacing the thermal gas leaving cavities filled with radio emission. The cavities are apparently supported against the local gas pressure by magnetic fields and cosmic rays. In addition, radio-faint, ``ghost'' cavities are seen in some clusters. They may be relics of earlier radio outbursts rising buoyantly in the intracluster medium. The radio sources may reduce the mass deposition rates by mechanical heating, and by inducing convective currents that move cool material outward.
dc.description11 pages, LaTeX, 1 color figure, presented at ``Constructing the Universe with Clusters of Galaxies,''IAP, Paris, France, 4-8 July, 2000
dc.identifierhttps://arxiv.org/abs/astro-ph/0012331
dc.identifierhttp://arxiv.org/abs/astro-ph/0012331
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/2230
dc.subjectAstrophysics
dc.titleNew Perspectives on Cooling Flows and Cluster Radio Sources
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