Gravitational waves from magnetorotational core-collapse supernovae using 3D GRMHD simulations: effect of rotation and magnetic fields

ABSTRACT We investigate the gravitational wave emission for 10 supernova progenitors from magnetorotational core-collapse to the supernova explosion using fully three-dimensional dynamical-space–time general-relativistic magnetohydrodynamics simulations with the GPU-accelerated (graphics processing unit-accelerated) code GRaM-X. We consider two progenitors of zero-age-main-sequence mass $25\,{\rm M}_{\odot }$ and eight with zero-age-main-sequence masses of $35\,{{\rm M}_{\odot }}$. For these models, we explore a range of rotation rates between 0.0 and $3.5 \, \mathrm{rad}\, \mathrm{s}^{-1}$, along with initial seed magnetic field of either $10^{12}\,\mathrm{G}$ or $10^{13}\,\mathrm{G}$. The analysis of the 10 models presented provides a comprehensive and systematic initial investigation of the interplay between progenitor rotation, magnetic field strength, and progenitor structure in shaping the explosion dynamics and gravitational wave (GW) emission. We find that stronger seed magnetic fields ($10^{13}\,\mathrm{G}$) suppress the GW strain amplitude relative to models with weaker initial fields ($10^{12}\,\mathrm{G}$). Increasing the initial rotation rate results in a more dynamical explosion, yielding correspondingly stronger gravitational waves. In addition, the progenitor mass/composition also exhibit a significant impact on the explosion dynamics and the morphology of the resulting waveforms. Finally, we find that all of our models lie above the detectability threshold for third generation detectors Advanced Laser Interferometer Gravitational-Wave Observatory (aLIGO), Einstein Telescope, and Cosmic explorer at a $10\,\mathrm{kpc}$ distance and most would even still be detectable at $\mathcal {O}(1)\mathrm{Mpc}$, opening the possibility for observing gravitational wave emission for CCSNe (core-collapse supernovae) beyond our Galaxy.