Numerical relativity simulations of charged black hole mergers demonstrate identical gravitational dynamics across electromagnetic duality rotations, with electromagnetic radiation polarization rotated by the duality angle.
A simple construction of initial data for multiple black holes
9 Pith papers cite this work. Polarity classification is still indexing.
9
Pith papers citing it
abstract
We consider the initial data problem for several black holes in vacuum with arbitrary momenta and spins on a three space with punctures. We compactify the internal asymptotically flat regions to obtain a computational domain without inner boundaries. When treated numerically, this leads to a significant simplification over the conventional approach which is based on throats and isometry conditions. In this new setting it is possible to obtain existence and uniqueness of solutions to the Hamiltonian constraint.
citation-role summary
background 1
citation-polarity summary
roles
background 1polarities
unclear 1representative citing papers
Ultra-relativistic black hole flybys can radiate over 65% of their energy in gravitational waves via irregular waveforms caused by radiation trapping and lensing, without coalescence.
Numerical relativity in the decoupling limit reveals dynamical scalarization and spin-induced (de)scalarization during hyperbolic black hole encounters for both signs of the coupling.
A new numerical relativity-inspired method achieves exponential convergence for scalar self-force calculations in Kerr spacetime on circular equatorial orbits up to near-extremal spins and the ISCO.
Scattering black holes gain spin and mass by absorbing emitted gravitational radiation, with spin-up up to 0.3 and mass gain up to 15% in near-threshold encounters.
PINNs with specialized techniques solve the nonlinear Hamiltonian constraint for generic binary black hole initial data, matching traditional NR accuracy.
Bayesian parameter estimation with targeted eccentric numerical-relativity waveforms yields eccentricity estimates of e20 ≈ 0.2 for GW200208_22 and e10 ≈ 0.19 for GW190620, reinforcing the eccentric hypothesis.
A grid-based multi-grid Poisson solver is implemented in numerical relativity, tested on puncture black holes and neutron stars, and used in a neutrino-radiation hydrodynamics simulation of 9 solar mass star collapse up to core bounce with high conservation accuracy.
Numerical relativity solved the general-relativistic two-body problem in the mid-2000s, supplying the waveform models that enabled LIGO's first gravitational-wave detections.
citing papers explorer
-
Electromagnetic duality degeneracy in dynamical black hole mergers
Numerical relativity simulations of charged black hole mergers demonstrate identical gravitational dynamics across electromagnetic duality rotations, with electromagnetic radiation polarization rotated by the duality angle.
-
Trapping, Irregular Waveforms, and Efficient Radiation in Ultra-relativistic Black Hole Encounters
Ultra-relativistic black hole flybys can radiate over 65% of their energy in gravitational waves via irregular waveforms caused by radiation trapping and lensing, without coalescence.
-
Scalarization and descalarization in hyperbolic encounters of black holes
Numerical relativity in the decoupling limit reveals dynamical scalarization and spin-induced (de)scalarization during hyperbolic black hole encounters for both signs of the coupling.
-
Self-force calculations with numerical relativity methods
A new numerical relativity-inspired method achieves exponential convergence for scalar self-force calculations in Kerr spacetime on circular equatorial orbits up to near-extremal spins and the ISCO.
-
Spin-up and mass-gain in hyperbolic encounters of spinning black holes
Scattering black holes gain spin and mass by absorbing emitted gravitational radiation, with spin-up up to 0.3 and mass gain up to 15% in near-threshold encounters.
-
Solving Hamiltonian Constraint Equation with Physics-Informed Neural Networks
PINNs with specialized techniques solve the nonlinear Hamiltonian constraint for generic binary black hole initial data, matching traditional NR accuracy.
-
Parameter Estimation with Targeted Eccentric Numerical-Relativity Simulations for GW200208_22 and GW190620
Bayesian parameter estimation with targeted eccentric numerical-relativity waveforms yields eccentricity estimates of e20 ≈ 0.2 for GW200208_22 and e10 ≈ 0.19 for GW190620, reinforcing the eccentric hypothesis.
-
Implementation of multi-grid Poisson solver in numerical relativity and its application to gravitational collapse of massive star
A grid-based multi-grid Poisson solver is implemented in numerical relativity, tested on puncture black holes and neutron stars, and used in a neutrino-radiation hydrodynamics simulation of 9 solar mass star collapse up to core bounce with high conservation accuracy.
-
The Era of Precision in Computational Models of Gravitational Waves
Numerical relativity solved the general-relativistic two-body problem in the mid-2000s, supplying the waveform models that enabled LIGO's first gravitational-wave detections.