Metal mixing by buoyant bubbles in galaxy clusters

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dc.creatorRoediger, E.
dc.creatorBrueggen, M.
dc.creatorRebusco, P.
dc.creatorBoehringer, H.
dc.creatorChurazov, E.
dc.date2006-11-16
dc.date.accessioned2026-07-07T10:20:51Z
dc.date.available2026-07-07T10:20:51Z
dc.descriptionUsing a series of three-dimensional, hydrodynamic simulations on an adaptive grid, we have performed a systematic study on the effect of bubble-induced motions on metallicity profiles in clusters of galaxies. In particular, we have studied the dependence on the bubble size and position, the recurrence times of the bubbles, the way these bubbles are inflated and the underlying cluster profile. We find that in hydrostatic cluster models, the resulting metal distribution is very elongated along the direction of the bubbles. Anisotropies in the cluster or ambient motions are needed if the metal distribution is to be spherical. In order to parametrise the metal transport by bubbles, we compute effective diffusion coefficients. The diffusion coefficients inferred from our simple experiments lie at values of around $\sim 10^{29}$ cm$^2$s$^{-1}$ at a radius of 10 kpc. The runs modelled on the Perseus cluster yield diffusion coefficients that agree very well with those inferred from observations.
dc.description17 pages, 12 figures. Accepted by MNRAS
dc.identifierhttps://arxiv.org/abs/astro-ph/0611531
dc.identifierhttp://arxiv.org/abs/astro-ph/0611531
dc.identifierMon.Not.Roy.Astron.Soc.375:15-28,2007
dc.identifierdoi:10.1111/j.1365-2966.2006.11300.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/174984
dc.subjectAstrophysics
dc.titleMetal mixing by buoyant bubbles in galaxy clusters
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