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

We present a series of fully three-dimensional high-resolution dynamical-spacetime general-relativistic magnetohydrodynamics (GRMHD) simulations of core-collapse supernovae (CCSNe) for a progenitor of zero-age main-sequence (ZAMS) mass 25M_⊙⁠. We simulate a total of 12 models 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 GRaM-X for magnetic fields B₀ = (10¹¹, 10¹²) G and rotation rates Ω0 = (0.14, 0.5, 1.0, 1.5, 2.0, 25) rad s^-1⁠. We find that models with B₀ = 10¹¹ G fail to explode, while those with B₀ = 10¹² G show a wide range of jet morphologies and explosive outcomes depending on the rotation rate. Models with B₀ = 10¹² G⁠, which have Ω₀ = (0.14, 0.5) rad s^-1⁠, also fail to explode. Models with B₀ = 1012 G and Ω₀ = (1.0, 1.5) rad S^-1 form tilted jets, giving the ejecta a more spherical character, but one also different from predominantly neutrino-driven explosions. Models with B₀ = 10¹² G and Ω₀ ≥ 2.0 rad s^-1 form jets that show ejecta velocities ≳ 15 000 km s-1⁠, making them suitable candidates for broad-lined Type Ic supernova progenitors. We also perform comparison lower resolution simulations. While average shock radii, protoneutron star (PNS) magnetic fields, PNS rotation rates, and the kink instability have similar behaviour as in high-resolution simulations, the ejecta mass and energy are
times lower. This work represents the largest set of 3D GRMHD simulations studying magnetorotational supernovae in full GR and demonstrates the potential of systematic studies with GPU-accelerated 3D simulations of CCSNe.