A new projector-based formalism determines effective potentials from perturbative amplitudes and resums them to compute non-perturbative gravitational waveforms for generic two-body trajectories.
Hawking Radiation from the Double Copy,
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Biadjoint scalar theory admits a family of non-topological solitons carrying U(1) charge, time-dependent like Q-balls, stable in truncation, with finite localized energy.
An on-shell framework derives local detailed balance and the black hole thermal spectrum from spin universality and unitarity.
The Smarr formula is structurally identical to the single-copy Gauss's law for Kerr-Schild black holes, with the AdS pressure-volume term arising from gauge background subtraction.
Noncommutative spacetime shifts the collapsing shell proportionally to outgoing Hawking mode momentum, invalidating standard robustness arguments and causing radiation to decay exponentially after scrambling for exponentially long black hole evaporation.
citing papers explorer
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Resumming Scattering Amplitudes for Waveforms
A new projector-based formalism determines effective potentials from perturbative amplitudes and resums them to compute non-perturbative gravitational waveforms for generic two-body trajectories.
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Non-topological solitons in biadjoint scalar field theory
Biadjoint scalar theory admits a family of non-topological solitons carrying U(1) charge, time-dependent like Q-balls, stable in truncation, with finite localized energy.
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Black Hole Thermodynamics Meets On-Shell Amplitudes: Local Detailed Balance and Thermal Spectrum from Spin Universality and Unitarity
An on-shell framework derives local detailed balance and the black hole thermal spectrum from spin universality and unitarity.
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The Smarr Formula is Gauss's Law: A Kerr-Schild Single-Copy Perspective
The Smarr formula is structurally identical to the single-copy Gauss's law for Kerr-Schild black holes, with the AdS pressure-volume term arising from gauge background subtraction.
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Exponentially Long Evaporation of Noncommutative Black Hole
Noncommutative spacetime shifts the collapsing shell proportionally to outgoing Hawking mode momentum, invalidating standard robustness arguments and causing radiation to decay exponentially after scrambling for exponentially long black hole evaporation.