Generic Dirichlet-wall spacetimes can end in finite-time spacelike singularities at the wall, including walls that fall into BTZ black holes.
Eardley and S.B
7 Pith papers cite this work, alongside 472 external citations. Polarity classification is still indexing.
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abstract
We investigate classical formation of a D-dimensional black hole in a high energy collision of two particles. The existence of an apparent horizon is related to the solution of an unusual boundary-value problem for Poisson's equation in flat space. For sufficiently small impact parameter, we construct solutions giving such apparent horizons in D=4. These supply improved estimates of the classical cross-section for black hole production, and of the mass of the resulting black holes. We also argue that a horizon can be found in a region of weak curvature, suggesting that these solutions are valid starting points for a semiclassical analysis of quantum black hole formation.
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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.
In linearized gravity, the plane-fronted shockwave from an ultrarelativistic particle hitting a massive particle at rest generates a secondary spherical gravitational shockwave whose amplitude and the collision's gravitational radiation flux are derived analytically.
Nonlocal form factors in D-dimensional gravity yield effective geometries whose nonlinear completion gives regular, asymptotically flat Schwarzschild deformations with de Sitter cores.
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.
Upper limits on ADD black hole mass MB at 14 TeV LHC range from 11.83 TeV (ζ=0, D=3, ΛD=1 TeV) down to 7.65 TeV (ζ=0.35), with similar shifts for D=7 and higher ΛD.
citing papers explorer
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Dirichlet walls and the end of time
Generic Dirichlet-wall spacetimes can end in finite-time spacelike singularities at the wall, including walls that fall into BTZ black holes.
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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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Gravitational Waves in High Energy Fixed-Target Collisions
In linearized gravity, the plane-fronted shockwave from an ultrarelativistic particle hitting a massive particle at rest generates a secondary spherical gravitational shockwave whose amplitude and the collision's gravitational radiation flux are derived analytically.
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Eikonal, nonlocality and regular black holes
Nonlocal form factors in D-dimensional gravity yield effective geometries whose nonlinear completion gives regular, asymptotically flat Schwarzschild deformations with de Sitter cores.
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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.
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Constraining ADD black holes at the LHC with $\sqrt{s} = 14$ TeV
Upper limits on ADD black hole mass MB at 14 TeV LHC range from 11.83 TeV (ζ=0, D=3, ΛD=1 TeV) down to 7.65 TeV (ζ=0.35), with similar shifts for D=7 and higher ΛD.
- Black Hole Response Theory and its Exact Shockwave Limit