A Black Hole is Born: 3D GRMHD Simulation of Black Hole Formation from Core-Collapse

Abstract

We present the first three-dimensional, fully general-relativistic magnetohydrodynamic (3D GRMHD) simulation of a black hole (BH) formed from the collapsed core of a massive star. The ability to self-consistently capture the birth of a compact remnant in 3D is crucial for modeling natal BH properties (including masses, spins, and kicks), which are of particular interest in the era of gravitational wave astronomy. However, such simulations have remained elusive due to extreme computational challenges and demands. We employ the GPU-accelerated dynamical-spacetime GRMHD code GRaM-X to follow the collapse, core-bounce, shock propagation, and eventual BH formation of a massive stellar progenitor in full 3D. We initialize our simulation by mapping a one-dimensional (1D) model of a star with a zero-age-main-sequence mass of $45M_{\odot }$ to 3D. We use moderate rotation (consistent with expectations from stellar evolution modeling) and a relatively weak dipolar magnetic field. The collapsing core drives a shock that reaches a maximum radius of roughly 170 km before stalling and does not lead to a successful explosion. The proto-neutron star accretes matter before collapsing to form a BH $t_{BH}\approx 325$ ms after core-bounce. The time of BH formation and initial BH mass are remarkably similar to those obtained with GR1D, a 1D general-relativistic neutrino-hydrodynamics code, to which we compare our results. We track the horizon of the newborn BH after formation and calculate a steady kick velocity of $v_{kick}\approx 72$ km/s and a mass of $M_{BH}\approx 2.62M_{\odot }$, which is still rising at the end of the simulation.

10 pages, 5 figures; accepted to ApJL

References in corpus (22)

• Modules for Experiments in Stellar Astrophysics (MESA)
• Delayed neutrino-driven supernova explosions aided by the standing accretion-shock instability
• Magnetorotational Core-Collapse Supernovae in Three Dimensions
• Neutron star kicks by the gravitational tug-boat mechanism in asymmetric supernova explosions: progenitor and explosion dependence
• Why binary interaction does not necessarily dominate the formation of Wolf-Rayet stars at low metallicity
• Black hole to breakout: 3D GRMHD simulations of collapsar jets reveal a wide range of transients
• A new general relativistic magnetohydrodynamics code for dynamical spacetimes
• The Collapse and Three-Dimensional Explosion of Three-Dimensional, vis à vis One-Dimensional, Massive-star Supernova Progenitor Models
• The Essential Character of the Neutrino Mechanism of Core-Collapse Supernova Explosions
• Three-dimensional core-collapse supernovae with complex magnetic structures: I. Explosion dynamics
• General Relativistic Hydrodynamic Simulations and Linear Analysis of the Standing Accretion Shock Instability around a Black Hole
• Pre-collapse Properties of Superluminous Supernovae and Long Gamma-Ray Burst Progenitor Models
• Three dimensional magnetorotational core-collapse supernova explosions of a 39 solar mass progenitor star
• Emission lines due to ionizing radiation from a compact object in the remnant of Supernova 1987A
• Standing Accretion Shocks in the Supernova Core: Effects of Convection and Realistic EOS
• Three-dimensional GRMHD Simulations of Rapidly Rotating Stellar Core-Collapse
• General Relativistic Neutrino-Driven Turbulence in One-Dimensional Core-Collapse Supernovae
• GRaM-X: A new GPU-accelerated dynamical spacetime GRMHD code for Exascale computing with the Einstein Toolkit
• Magnetically-Driven Neutron-Rich Ejecta Unleashed: Global 3D Neutrino-General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
• Density Profiles of Collapsed Rotating Massive Stars Favor Long Gamma-Ray Bursts
• AsterX: a new open-source GPU-accelerated GRMHD code for dynamical spacetimes
• Numerical relativity simulations of black hole and relativistic jet formation