Three-dimensional Magneto-hydrodynamic Simulations of Core-collapse Supernovae: I. Hydrodynamic evolution and protoneutron star properties

Understand

We present results from three-dimensional, magnetohydrodynamic, core-collapse simulations of sixteen progenitors following until 0.5 s after bounce.

• We use non-rotating solar-metallicity progenitor models with zero-age main-sequence mass between 9 and 24 $M_{\odot}$.
• The examined progenitors cover a wide range of the compactness parameter including a peak around $23 M_{\odot}$.
• We find that neutrino-driven explosions occur for all models within 0.3 s after bounce.