MHD in galaxy clusters

Galaxy groups and clusters provide a laboratory for diverse physical phenomena such as MHD on large scales Subsonic through supersonic flows around merging clumps and tangential discontinuities magnetize the plasma in some cases to gt 10 levels So far an analytic solution for the compressible flow in front of a moving clump or any local prescription for magnetization in a general flow have not been available In this talk I will present such solutions In particular I will show that parameterizing space using path or