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The radio lobes of Hydra A lie within cavities surrounded by a rim ofenhanced X-ray emission in the intracluster gas. Although the bright rimappears cooler than the surrounding gas, existing Chandra data do not excludethe possibility that the rim is produced by a weak shock. A temperature mapshows that cool gas extends out along the radio axis of Hydra A. The age of theradio source and equipartition pressure of the radio lobe argue against ashock, and comparison with similar structure in the Perseus Cluster alsosuggests that the rim is cool. We show that the cool bright rim cannot be theresult of shock induced cooling, or due to the effect of magnetic fields inshocks. The most likely source of low entropy (cool) gas is entrainment by therising cavity. This requires some means of communicating the bouyant force onthe cavity to the surrounding gas. The magnetic field required to produce theFaraday rotation in Hydra A has the appropriate properties for this, if theFaraday screen is mainly in this bright rim. In Hydra A, the mass outflow dueto the rising cavities could be sufficient to balance cooling driven inflow, sopreventing the build up of low entropy gas in the cluster core.Comment: 28 pages, LaTeX, 9 figures, accepted for publication in Ap

Interaction of Radio Lobes with the Hot Intracluster Medium: Driving Convective Outflow in Hydra A