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Primary black-hole scalar charges and kinetic screening in $K$-essence-Gauss-Bonnet gravity
General Relativity and Quantum Cosmology · Submitted 29 Dec 2025
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We then turn to the case where self-accelerating cosmology is driven by $K(X)$, finding that the time-dependence of the scalar field opens up the parameter space, turning the black-hole scalar charge from secondary to primary.
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The abstract, sentence by sentence
Black holes beyond General Relativity may carry non-standard charges that impact their phenomenology. We study how the scalar charge that is induced by the scalar-Gauss-Bonnet coupling is affected by the presence of a nontrivial kinetic term $K(X)$ in a test-field approximation. We discuss the corresponding kinetic screening in the asymptotically flat, static solution first. We then turn to the case where self-accelerating cosmology is driven by $K(X)$, finding that the time-dependence of the scalar field opens up the parameter space, turning the black-hole scalar charge from secondary to primary. We provide a stability analysis and a measure of the intensity of the kinetic screening from the quartic dispersion relation of the mixed scalar and gravitational modes.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Black holes beyond General Relativity may carry non-standard charges that impact their phenomenology. | background 1.00 | 0.04 | 0.04 | hedged possibility 1.00 |
| s1 | We study how the scalar charge that is induced by the scalar-Gauss-Bonnet coupling is affected by the presence of a nontrivial kinetic term $K(X)$ in a test-field approximation. | contribution 0.99 | 0.90 | 0.08 | asserted 0.79 |
| s2 | We discuss the corresponding kinetic screening in the asymptotically flat, static solution first. | contribution 0.67 | 0.83 | 0.04 | unclear 0.51 |
| s3 | We then turn to the case where self-accelerating cosmology is driven by $K(X)$, finding that the time-dependence of the scalar field opens up the parameter space, turning the black-hole scalar charge from secondary to primary. | result 0.93 | 0.94 | 0.68 | asserted 1.00 |
| s4 | We provide a stability analysis and a measure of the intensity of the kinetic screening from the quartic dispersion relation of the mixed scalar and gravitational modes. | contribution 0.69 | 0.95 | 0.08 | asserted 1.00 |
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The paper
Original abstract
Black holes beyond General Relativity may carry non-standard charges that impact their phenomenology. We study how the scalar charge that is induced by the scalar-Gauss-Bonnet coupling is affected by the presence of a nontrivial kinetic term $K(X)$ in a test-field approximation. We discuss the corresponding kinetic screening in the asymptotically flat, static solution first. We then turn to the case where self-accelerating cosmology is driven by $K(X)$, finding that the time-dependence of the scalar field opens up the parameter space, turning the black-hole scalar charge from secondary to primary. We provide a stability analysis and a measure of the intensity of the kinetic screening from the quartic dispersion relation of the mixed scalar and gravitational modes.
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References
How the literature uses it
1 arXiv paper cite this in 1 sentence
What it cites · 60 sentences without a confident label
Uses the method or tool of 5 papers
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Following e.g. [ref] (see also e.g. [ref] in the context of acoustic geometry or [ref] in the context of quasinormal modes beyond GR), we introduce a small parameter $ϵ$ that controls the ratio between the wavelength of the perturbations and the characteristic length scale of the background and write [equation] This approximation is valid for rapidly oscillating perturbations whose wavelengths are much shorter than the scale over which the background varies.
Analogue Gravity · Demixing the system of equations, dispersion relations and the characteristic invariant · 0.95
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Following e.g. [ref] (see also e.g. [ref] in the context of acoustic geometry or [ref] in the context of quasinormal modes beyond GR), we introduce a small parameter $ϵ$ that controls the ratio between the wavelength of the perturbations and the characteristic length scale of the background and write [equation] This approximation is valid for rapidly oscillating perturbations whose wavelengths are much shorter than the scale over which the background varies.
Eikonal quasinormal modes of black holes beyond general relativity III: scalar Gauss-Bonnet gravity · Demixing the system of equations, dispersion relations and the characteristic invariant · 0.95
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Following e.g. [ref] (see also e.g. [ref] in the context of acoustic geometry or [ref] in the context of quasinormal modes beyond GR), we introduce a small parameter $ϵ$ that controls the ratio between the wavelength of the perturbations and the characteristic length scale of the background and write [equation] This approximation is valid for rapidly oscillating perturbations whose wavelengths are much shorter than the scale over which the background varies.
2412.21169 · Demixing the system of equations, dispersion relations and the characteristic invariant · 0.95
Compares with 1 paper
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A direct comparison between the cosmological and EFT quantities shows that they coincide once a gauge factor $Γ≡- q_c/H M_*^2 (2 - α_B)$ is introduced to account for the choice of unitary gauge adopted in Ref. [ref] .
Maximal freedom at minimum cost: linear large-scale structure in general modifications of gravity · Limiting cases · 0.91
Cites as background 27 papers
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Let us look for self-accelerating solutions in cosmology in this model in a very simplistic approach that will be sufficient for our purposes —other realizations are possible, see e.g. Ref. [ref] .
K-mouflage Cosmology: the Background Evolution · Homogeneous cosmology · 0.90
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It was subsequently realized that all these models fall within the Horndeski class [ref] , the most general scalar-tensor theory with second order field equations, later extended to include degenerate higher-order scalar-tensor theories that avoid the propagation of additional degrees of freedom (d.o.f.) [ref] —for reviews see Refs. [ref] .
Third order equations of motion and the Ostrogradsky instability · Introduction · 0.94
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It was subsequently realized that all these models fall within the Horndeski class [ref] , the most general scalar-tensor theory with second order field equations, later extended to include degenerate higher-order scalar-tensor theories that avoid the propagation of additional degrees of freedom (d.o.f.) [ref] —for reviews see Refs. [ref] .
Degenerate higher derivative theories beyond Horndeski: evading the Ostrogradski instability · Introduction · 0.94
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