1. Visualization of Simulated White Dwarf Collisions as a Primary Channel for Type Ia Supernovae

2. Overview
PI: Doron Kushnir, Institute for Advanced Study, Weizmann Institute
ECSS: David Bock, National Center for Supercomputing Applications
Type Ia supernovae created by thermonuclear explosions of white dwarf stars
What causes the thermonuclear explosion remains an open question
Direct collisions of white dwarf stars at extreme velocities could be the answer
56Ni (nickel) distribution is an observed characteristic of Type Ia supernovae
Conclusions can be made if collisions achieve an ignition and reproduce 56Ni

3. Simulation Data 3D adaptive mesh refinement, FLASH HDF5
Varying number of 16^3 data blocks (~5 to ~140,000)
Scalar variables: density, temperature, 56Ni

4. Simulation Data Write converter to custom system format
Remove blocks containing only minimum data values
Convert from cell-centered to node-centered

5. Visualization 2D color-mapped slice animation tests
Slice plane through middle of AMR boundary grid
Density, temperature

6. Visualization 3D volume rendering animation tests
Applying different transfer curves, different structures

7. Visualization 3D volume rendering animation tests
Attempt to show both outer and inner structures

8. Visualization 3D volume rendering animation tests
Exterior view of density, demonstrate collision area

9. Visualization 3D volume rendering animation tests
Exterior view of density, demonstrate collision area

10. Visualization
3D volume rendering animation tests
Temperature and 56Ni

11. Visualization Show 56Ni within temperature field
Final XSEDE16 Visualization Showcase