Open Access3D SIMULATIONS OF RADIO GALAXY EVOLUTION IN CLUSTER MEDIA
Author(s) -
Sean O’Neill,
Paul Shearer,
I. L. Tregillis,
T. W. Jones,
Dongsu Ryu
Publication year - 2004
Publication title -
journal of the korean astronomical society/journal of the korean astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.568
H-Index - 22
eISSN - 2288-890X
pISSN - 1225-4614
DOI - 10.5303/jkas.2004.37.5.605
Subject(s) - physics , mach number , intracluster medium , cluster (spacecraft) , astrophysics , jet (fluid) , radius , galaxy cluster , kinetic energy , supersonic speed , thermal , magnetohydrodynamics , computational physics , mechanics , galaxy , plasma , meteorology , classical mechanics , computer security , computer science , programming language , quantum mechanics
We present a set of high-resolution 3D MHD simulations exploring the evolution of light, supersonic jets in cluster environments. We model sets of high- and low-Mach jets entering both uniform surroundings and King-type atmospheres and propagating distances more than 100 times the initial jet radius. Through complimentary analyses of synthetic observations and energy flow, we explore the detailed interactions between these jets and their environments. We find that jet cocoon morphology is strongly influenced by the structure of the ambient medium. Jets moving into uniform atmospheres have more pronounced backflow than their non-uniform counterparts, and this difference is clearly reflected by morphological differences in the synthetic observations. Additionally, synthetic observations illustrate differences in the appearances of terminal hotspots and the x-ray and radio correlations between the high- and low-Mach runs. Exploration of energy flow in these systems illustrates the general conversion of kinetic to thermal and magnetic energy in all of our simulations. Specifically, we examine conversion of energy type and the spatial transport of energy to the ambient medium. Determination of the evolution of the energy distribution in these objects will enhance our understanding of the role of AGN feedback in cluster environments.clos