Three-dimensional GRMHD Simulations of Rapidly Rotating Stellar Core-Collapse

Understand

We present results from fully general relativistic (GR), three-dimensional (3D), neutrino-radiation magneto-hydrodynamic (MHD) simulations of stellar core collapse of a 20 M$_\odot$ star with spectral neutrino transport.

• Our focus is to study the gravitational-wave (GW) signatures from the magnetorotationally (MR)-driven models.
• By parametrically changing the initial angular velocity and the strength of the magnetic fields in the core, we compute four models.
• Our results show that the MHD outflows are produced only for models (two out of four), to which magnetic field strengths of 10$^{12}$ G and rotation rates of 1 or 2 rad s$^{-1}$ are initially imposed in the core.