Physics
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21622103p&link_type=abstract
American Astronomical Society, AAS Meeting #216, #221.03; Bulletin of the American Astronomical Society, Vol. 41, p.893
Physics
Scientific paper
X-ray and radio observations of galaxy clusters have revealed a wealth of structures in the intra-cluster medium (ICM), many of which caused by extra-galactic radio sources powered by AGNs. Structures in the form of large X-ray cavities (often coincide with radio jets and lobes) and weak shocks (often associated with jet/lobe expansion) have provided a reliable gauge of the energy output from AGNs. This energy has often been considered as crucial in understanding the AGN feedback process in the ICM. The rich variety of observed morphologies of extra-galactic radio jets/lobes in galaxy clusters has highlighted the need of understanding how magnetized jet/lobe plasmas interact with the background ICM. These observations have revealed interesting new questions and constraints on the properties of jets and lobes. We will present 3-D magnetohydrodynamics (MHD) simulations to study the large scale structures of jets/lobes in the ICM and make direct comparisons with observations, esp. those in radio and X-rays. How jets/lobes terminate in the ICM depends on the form of the energy jets carry (e.g., kinetic, magnetic or thermal). This in turn determines the morphology and size of X-ray cavities, against which jet/lobe MHD simulations could be tested. Furthermore, the jet/lobe properties on these large scales can provide insights on how the jet properties (its speed, composition, global current, etc.) evolve from the black-hole accretion disk scale ( AU) to termination ( hundreds of kpc to a few Mpc). The improved understanding in this aspect provides more physics underpinning for modeling AGN feedbacks in clusters. Implications for magnetic fields in galaxy clusters will be discussed as well.
(Supported by DOE/OFES and LDRD program at LANL).
Li Handong
Pino Jesse
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