Clumps With Self Contained Magnetic Field And Their Interaction With Shocks Shule Li, Adam Frank, Eric Blackman University of Rochester, Department of Physics and Astronomy. Rochester, New York 14627

Introduction Problem of clumps and their interaction with shocks is crucial in understanding interstellar medium, supernova remnants etc. Magnetic field often plays an important role in such an interaction. Most previous numerical studies focuse on clumps immersed in a uniform background magnetic field. However, realistic clumps usually contain tangled magnetic field inside them. Our study focus on clump's shocked behavior when there is a tangled magnetic field contained. The field's spatial distribution can be either ordered or random. wind ambient clump Problem Description

Previous Works Field aligned with shock Magnetic field is amplified at the top of and behind the clump. The top of the shocked clump is streamlined but there is no significant suppression on the fragmentation of the clump even for low initial β cases. Field perpendicular with shock Magnetic field is wrapping around the clump and gets greatly amplified due to stretching. The shocked clump is highly streamlined and the fragmentation can be greatly suppressed even for high initial β cases. Jones, T.W., Ryu, Dongsu, Tregillis, I.L. 1996 ApJ, 473, 365 Adding radiative cooling into the simulation can further change the shocked behavior: more thin fragments, confined boundary flows, etc. (Fragile et al, 2005 ApJ 619, 327)

AstroBEAR is a parallelized hydrodynamic/MHD simulation code suitable for a variety of astrophysical problems. AstroBEAR is designed for 2D and 3D adaptive mesh refinement (AMR) simulations, the current versioncode shows good scaling results up to 2000 processors. In addition, AstroBEAR comes with a number of multiphysical processes such as self gravity, thermal conduction and resistivity.

Simulation Setup Density Contrast Wind Mach Alfvenic Mach Magnetic Beta Crushing Time Toroidal. Aligned Poloidal. Perp. Poloidal. Aligned The simulation is set up so that the wind crossing time is shorter than the Alfvenic crossing time, the latter is shorter than the sound crossing time. We investigate the case when the contained field is ordered, as well as the case when the contained field is random. Radiative cooling is included in the simulation.

Movie: Toroidal Perpendicular

Movie: Toroidal Aligned

Movie: Poloidal Perpendicular

Movie: Poloidal Aligned

Movie: Random Field with Kolmogorov Type Spectrum

Discussion I: Clump Morphology When the toroidal field is aligned with the shock, the clump material are compressed into a “nose cone”shape bounded by strong toroidal field. This phenomenon is similar to the “nose cone”shapes seen in MHD jet simulations. If we add a weak poloidal field to the above toroidal field, we see a much thicker “nose cone” with a ring shaped head. It is because even a weak added poloidal field can break the axisymmetry.

Discussion I: Clump Morphology The direction of field pinch will affect the clump's morphological evolution.

Discussion II: Mixing Ratio The initial field geometry affects the mixing ratio. The poloidal aligned case has the most magnetic energy in field component aligned with the shock direction; the two perpendicular cases only have a part of their magnetic energy in the field component aligned with the shock direction; the toroidal aligned case has no such component at all.

Discussion II: Kinetic Energy Transport Mixing ratio and kinetic energy transport are correlated. More aligned field components results in higher mixing ratio, more efficient clump fragmentation, higher kinetic transport efficiency and more turbulent downstream flow.

Summary

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