Heating cooling flows with jets

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dc.creatorOmma, Henrik
dc.creatorBinney, James
dc.creatorBryan, Greg
dc.creatorSlyz, Adrianne
dc.date2003-07-27
dc.date2003-11-11
dc.date.accessioned2026-07-07T10:27:01Z
dc.date.available2026-07-07T10:27:01Z
dc.descriptionActive galactic nuclei are clearly heating gas in `cooling flows'. The effectiveness and spatial distribution of the heating are controversial. We use three-dimensional simulations on adaptive grids to study the impact on a cooling flow of weak, subrelativistic jets. The simulations show cavities and vortex rings as in the observations. The cavities are fast-expanding dynamical objects rather than buoyant bubbles as previously modelled, but shocks still remain extremely hard to detect with X-rays. At late times the cavities turn into overdensities that strongly excite the cluster's g-modes. These modes damp on a long timescale. Radial mixing is shown to be an important phenomenon, but the jets weaken the metallicity gradient only very near the centre. The central entropy density is modestly increased by the jets. We use a novel algorithm to impose the jets on the simulations.
dc.description16 pages, 15 figures. Accepted for publication in MNRAS. Revised version taking referee's comments into account, minor changes. High-resolution version and MPEGs can be found at http://www.clusterheating.org/papers.php
dc.identifierhttps://arxiv.org/abs/astro-ph/0307471
dc.identifierhttp://arxiv.org/abs/astro-ph/0307471
dc.identifierMon.Not.Roy.Astron.Soc.348:1105,2004
dc.identifierdoi:10.1111/j.1365-2966.2004.07382.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/177035
dc.subjectAstrophysics
dc.titleHeating cooling flows with jets
dc.typetext

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