📝 SummarXiv

Abstract

We investigate the gravitational wave emission for 10 supernova progenitors from magnetorotational core-collapse to the supernova explosion using fully three-dimensional dynamical-spacetime general-relativistic magnetohydrodynamics simulations with the GPU-accelerated code $\texttt{GRaM-X}$. We consider 2 progenitors of zero-age-main-sequence mass $25M_\odot$ and 8 with zero-age-main-sequence masses of $35M_\odot$. 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 3rd generation detectors aLIGO, Einstein Telescope, and Cosmic explorer at a $10\mathrm{kpc}$ distance and most would even still be detectable at $10\mathrm{Mpc}$, opening the possibility for observing gravitational wave emission for CCSNe beyond our galaxy.