3D full-GR simulations of magnetorotational core-collapse supernovae on GPUs: A systematic study of rotation rates and magnetic fields

Abstract

We present a series of fully three-dimensional, dynamical-spacetime general relativistic magnetohydrodynamics (GRMHD) simulations of core-collapse supernovae (CCSNe) for a progenitor of zero-age-main-sequence (ZAMS) mass $25M_{\odot }$. We simulate a total of 12 models for simulation times in the range $190-260\mathrm{ms}$ to systematically study the effect of rotation rates and magnetic fields on jet formation via the magnetorotational mechanism. We have performed simulations on OLCF's Frontier using the new GPU-accelerated dynamical-spacetime GRMHD code \theCode for magnetic fields $B_0=(10^{11},10^{12})\mathrm{G}$ and rotation rates ${\Omega }_0=(0.14,0.5,1.0,1.5,2.0,2.5)rad/s$. We always resolve the entire region containing the shock with a resolution of at least $1.48\mathrm{km}$. We find that models with $B_0=10^{11}\mathrm{G}$ fail to explode, while those with $B_0=10^{12}\mathrm{G}$ show a wide range of jet morphologies and explosive outcomes depending on the rotation rate. Models with $B_0=10^{12}\mathrm{G}$ and ${\Omega }_0=(1.0,1.5)rad/s$ form jets that bend sideways, giving the ejecta a more spherical character, and possibly representing explosions that \textit{appear} neutrino-driven even though they are magnetorotationally-driven. Models with $B_0=10^{12}\mathrm{G}$ and ${\Omega }_0\ge 2.0rad/s$ show ejecta velocities $\gtrsim 15000km/s$, making them suitable candidates for broad-lined type Ic supernova progenitors. This work represents the largest set of 3D general-relativistic GRMHD simulations studying magnetorotational supernovae in full GR and demonstrates the potential of systematic studies with GPU-accelerated 3D simulations of CCSNe.

14 pages, 10 figures. Submitted to MNRAS

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