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We present results from deeper {\em Chandra} observations of the southwestradio lobe of Centaurus A, first described by Kraft et al. (2003). We find thatthe sharp X-ray surface brightness discontinuity extends around $\sim$75% ofthe periphery of the radio lobe, and detect significant temperature jumps inthe brightest regions of this discontinuity nearest to the nucleus. Thisdemonstrates that this discontinuity is indeed a strong shock which is theresult of an overpressure which has built up in the entire lobe over time.Additionally, we demonstrate that if the mean free path for ions to transferenergy and momentum to the electrons behind the shock is as large as theSpitzer value, the electron and proton temperatures will not have equilibratedalong the SW boundary of the radio lobe where the shock is strongest. Thus theproton temperature of the shocked gas could be considerably larger than theobserved electron temperature, and the total energy of the outburstcorrespondingly larger as well. We investigate this using a simpleone-dimensional shock model for a two-fluid (proton/electron) plasma. We findthat for the thermodynamic parameters of the Cen A shock the electrontemperature rises rapidly from $\sim$0.29 keV (the temperature of the ambientISM) to $\sim$3.5 keV at which point heating from the protons is balanced byadiabatic losses. The proton and electron temperatures do not equilibrate in atimescale less than the age of the lobe. We note that the measured electrontemperature of similar features in other nearby powerful radio galaxies in poorenvironments may considerably underestimate the strength and velocity of theshock.

astrophysical journal/the astrophysical journal

A Chandra Study of the Lobe/ISM Interactions Around the Inner Radio  Lobes of Centaurus A: Constraints on the Temperature Structure and Transport  Processes