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.
Black-hole binaries, gravitational waves, and numerical relativity
5 Pith papers cite this work. Polarity classification is still indexing.
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abstract
Understanding the predictions of general relativity for the dynamical interactions of two black holes has been a long-standing unsolved problem in theoretical physics. Black-hole mergers are monumental astrophysical events, releasing tremendous amounts of energy in the form of gravitational radiation, and are key sources for both ground- and space-based gravitational-wave detectors. The black-hole merger dynamics and the resulting gravitational waveforms can only be calculated through numerical simulations of Einstein's equations of general relativity. For many years, numerical relativists attempting to model these mergers encountered a host of problems, causing their codes to crash after just a fraction of a binary orbit could be simulated. Recently, however, a series of dramatic advances in numerical relativity has allowed stable, robust black-hole merger simulations. This remarkable progress in the rapidly maturing field of numerical relativity, and the new understanding of black-hole binary dynamics that is emerging is chronicled. Important applications of these fundamental physics results to astrophysics, to gravitational-wave astronomy, and in other areas are also discussed.
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Numerical study of cusp formation on horizons in head-on non-spinning black hole mergers, with analysis of mass and multipole behavior at the cusp and a proposed phenomenological model.
JWST observations of ERQs show stratified gas kinematics via deblended optical emission lines, with UV lines dominated by scattered light and optical lines mixing scattered and obscured emission.
A Gaussian Process Regression model trained on an archive of eccentricity-reduced binary black hole simulations predicts initial conditions that achieve low eccentricity with zero or one iteration.
Hydrodynamic drag makes BBH waveforms resemble higher-mass vacuum sources, biasing matched-filter chirp-mass estimates upward for LISA sources.
citing papers explorer
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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.
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Cusp Formation in Merging Black Hole Horizons
Numerical study of cusp formation on horizons in head-on non-spinning black hole mergers, with analysis of mass and multipole behavior at the cusp and a proposed phenomenological model.
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Kinematic Stratification in Extremely Red Quasars Revealed by JWST
JWST observations of ERQs show stratified gas kinematics via deblended optical emission lines, with UV lines dominated by scattered light and optical lines mixing scattered and obscured emission.
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Data-Driven Acceleration of Eccentricity Reduction for Binary Black Hole Simulations
A Gaussian Process Regression model trained on an archive of eccentricity-reduced binary black hole simulations predicts initial conditions that achieve low eccentricity with zero or one iteration.
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Retrieving the True Masses of Gravitational-wave Sources
Hydrodynamic drag makes BBH waveforms resemble higher-mass vacuum sources, biasing matched-filter chirp-mass estimates upward for LISA sources.