Journal
ASTROPHYSICAL JOURNAL
Volume 710, Issue 1, Pages 180-196Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/710/1/180
Keywords
galaxies: clusters: general; galaxies: jets; methods: numerical; magnetohydrodynamics (MHD)
Categories
Funding
- NSF [AST06-07674]
- University of Minnesota Supercomputing Institute
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0908668] Funding Source: National Science Foundation
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We report on a series of three-dimensional magnetohydrodynamic simulations of active galactic nucleus (AGN) jet propagation in realistic models of magnetized galaxy clusters. We are primarily interested in the details of energy transfer between jets and the intracluster medium (ICM) to help clarify what role such flows could have in the reheating of cluster cores. Our simulated jets feature a range of intermittency behaviors, including intermittent jets that periodically switch on and off and one model jet that shuts down completely, naturally creating a relic plume. The ICM into which these jets propagate incorporates tangled magnetic field geometries and density substructure designed to mimic some likely features of real galaxy clusters. We find that our jets are characteristically at least 60% efficient at transferring thermal energy to the ICM. Irreversible heat energy is not uniformly distributed, however, instead residing preferentially in regions very near the jet/cocoon boundaries. While intermittency affects the details of how, when, and where this energy is deposited, all of our models generically fail to heat the cluster cores uniformly. Both the detailed density structure and nominally weak magnetic fields in the ICM play interesting roles in perturbing the flows, particularly when the jets are non-steady. Still, this perturbation is never sufficient to isotropize the jet energy deposition, suggesting that some other ingredient is required for AGN jets to successfully reheat cluster cores.
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