Tracing gas motions in the Centaurus cluster |
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| Authors: | J Graham A C Fabian J S Sanders R G Morris |
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| Institution: | Institute of Astronomy, Madingley Road, Cambridge;Kavli Institute for Particle Astrophysics and Cosmology, Stanford Linear Accelerator Centre, Stanford, CA 94305-4060, USA |
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| Abstract: | We apply the stochastic model of iron transport developed by Rebusco et al. to the Centaurus cluster. Using this model, we find that an effective diffusion coefficient D in the range 2 × 1028–4 × 1028 cm2 s?1 can approximately reproduce the observed abundance distribution. Reproducing the flat central profile and sharp drop around 30–70 kpc , however, requires a diffusion coefficient that drops rapidly with radius so that D > 4 × 1028 cm2 s?1 only inside about 25 kpc . Assuming that all transport is due to fully developed turbulence, which is also responsible for offsetting cooling in the cluster core, we calculate the length- and velocity-scales of energy injection. These length-scales are found to be up to a factor of ～10 larger than expected if the turbulence is due to the inflation and rising of a bubble. We also calculate the turbulent thermal conductivity and find it is unlikely to be significant in preventing cooling. |
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| Keywords: | galaxies: clusters: general galaxies: clusters: individual: Centaurus cooling flows |
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