  We study the interaction of strong shock waves with magnetized clumps.
Previous numerical work focused on the simplified scenario in which shocked
clumps are immersed in a globally uniform magnetic field that extends through
both the clump and the ambient medium. Here we consider the complementary
circumstance in which the field is completely self-contained within the clumps.
This could arise naturally during clump formation via dynamical or thermal
instabilities for example as magnetic field pinches off from the ambient
medium. Using our AMR MHD code AstroBEAR, we carry out a series of simulations
with magnetized clumps that have different self-contained magnetic field
configurations. We find that the clump and magnetic evolution are sensitive to
the fraction of magnetic field aligned with versus perpendicular to the shock
normal. The relative strength of magnetic pressure and tension in the different
field configurations allows us to analytically understand the different cases
of post-shock evolution. We also show how turbulence and the mixing it implies
depends of the initial field configuration and suggest ways in which observed
shock-clump morphology may be used as a proxy for identifying internal field
topologies a posteriori.
