Speaker
Description
As they penetrate tens to hundreds of kpc through ICMs, AGN jets and their
back-flows often can highlight distinct ICM structures encountered along the
way. Those ICM structures frequently represent important, "tell-tale"
signatures of that cluster's environment and dynamical history, so of its
formation and evolution. Consequently, characterizing such AGN distortions
and, especially the physical properties of the associated ICM structures
encountered and their relationships to a cluster's dynamical history can
provide unique and valuable probes of cluster formation and ICM physics. In
this talk I will summarize some of the MHD simulations by our group that are
designed to refine understanding of these relationships. The simulations
include energy-dependent transport of cosmic ray electrons (CRe) and their
emissions needed to clearly establish unique and diagnostic signatures of these interactions.
Acknowledgements: This work was supported at the University of Minnesota by
NSF grant AST-1714205 and by the University of Minnesota Supercomputing
Institute. We also thank multiple contributors over the years to development
of the codes used in the simulations reported.
