Temporal & Spatial Evolution of a Modeled CME Shock and Post-shock Compression

We studied the temporal and spatial evolution of a modeled Coronal Mass Ejection (CME) driven shock and it's post-shock compression. Our goal has been to understand how the shock and the post-shock compression, as a whole with it's typical geometrical features, evolve over real time in different directions. We investigated how θ_Bn (the angle between the shock normal and the upstream magnetic field), Vs (shock velocity), Ms (Sonic Mach number), Ma (Alfven Mach number) evolve in real time at different locations on the shock and the post-shock surface. To do this, we used Rankine-Hugoniot (R-H) shock conditions of a 3D MHD shock and compared it with the other popular shock defining parameters. We also comment on the discrepancies and consequences on our observations. The CME has been initiated and then evolved in the lower solar corona with the help of Space Weather modeling Framework with a Titov- Demoulin (TD) type flux rope.