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

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

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

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

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

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

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

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

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

Visualization 3D volume rendering animation tests Temperature and 56Ni

Visualization Show 56Ni within temperature field Final XSEDE16 Visualization Showcase