Preliminary results from the first 3D simulation:

The shocked ejecta in our models reproduces the X-ray morphology of Cassiopeia A. The next step is to include tracking of the ionization state of the shocked gas in the simulation so that we can compute realistic models of the X-ray emission for detailed comparison with Chandra observations.

The evolution of the supernova remnant model can be seen in this animation. This 2D slice is projected in R-Theta coordinates (such that the spherical shock front now looks flat), and the color represents the logarithm of the gas density.

This 3D isosurface singles out the densest filaments of shocked ejecta, with the surface colored by gas temperature (red is hot, purple is cool). [Click on the image for an mpeg of this rotating image.]