From Jets to Failed Supernovae: Morphologies and Gravitational-Wave Signatures in Two-Dimensional Magnetorotational Core-Collapse Supernovae

TL;DR

This study conducts 34 two-dimensional magnetorotational core-collapse supernova simulations, revealing diverse explosion types, their dependence on initial conditions, and associated gravitational wave signatures, advancing understanding of supernova mechanisms and gravitational wave detection prospects.

Contribution

It systematically explores the effects of magnetic fields and rotation on supernova explosion morphologies, energies, and gravitational wave signals in a 40 solar mass progenitor model.

Findings

Failed explosions lead to black holes without magnetic fields.

Strong magnetic fields and rotation lower explosion thresholds.

Explosion energies can reach ~10^{51} erg, potential hypernovae.

Abstract

Magnetized and rotating core-collapse supernovae (CCSNe) are promising candidates for producing long gamma-ray bursts and hypernovae. In this project, we present 34 two-dimensional magnetized core-collapse supernova simulations with self-consistent neutrino transport, systematically exploring the parameter space of initial magnetic field strengths ($B_0 = 0$--$3.5 \times 10^{12}$~G) and rotation rates ($\Omega_0 = 0$--$0.5$~rad~s$^{-1}$) for a 40~$M_\odot$ progenitor. Our simulations reveal four distinct explosion morphologies: failed explosions leading to black hole formation, monopolar jet explosions, bipolar jet explosions, and neutrino-driven explosions. We find that the 40 $M_\odot$ progenitor model failed to explode without magnetic fields in two dimensions, even with rapid rotation. The non-rotating models require strong seed magnetic fields ($B_0 \gtrsim 1.5 \times 10^{12}$~G) to launch magnetically driven explosions, while the introduction of rotation substantially lowers this threshold. The explosion timescale decreases systematically with both increasing magnetic field strength and rotation rate, ranging from $>500$~ms in marginally successful models to $<150$~ms in strongly magnetized, rapidly rotating systems. Diagnostic explosion energies in the most extreme models approach $\sim 10^{51}$~erg within 250~ms and continue growing in time, making them potential hypernovae and long gamma-ray burst progenitors. Finally, we analyze the gravitational wave signatures associated with each morphology and find that the gravitational wave frequencies mainly depend on the rotation rates but are less sensitive to the magnetic field strengths and explosion morphologies. However, the gravitational wave amplitudes strongly depend on the explosion morphologies and magnetic fields, making searches for gravitational waves from magnetorotational core-collapse supernovae more challenging.