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Stabilization of the extended horizons
High Energy Physics - Theory · Submitted 27 May 2021
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The corresponding gravitational dual is ${\cal N}=2^*$ black brane with a dynamical instability of its translationary invariant horizon.
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The abstract, sentence by sentence
We extend Kodama-Ishibashi and Jansen-Rostworowski-Rutkowski master field framework to study quasinormal modes of black branes and black holes of Einstein gravity in $D=5$ space-time dimensions with multiple scalars and an arbitrary bulk potential. As an application, we consider a thermodynamically unstable state of mass deformed ${\cal N}=4$ supersymmetric Yang-Mills theory at strong coupling. The corresponding gravitational dual is ${\cal N}=2^*$ black brane with a dynamical instability of its translationary invariant horizon. We study the dependence of the quasinormal mode spectra as the boundary gauge theory is compactified on $S^3$ -- the black brane is turned into the black hole.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We extend Kodama-Ishibashi and Jansen-Rostworowski-Rutkowski master field framework to study quasinormal modes of black branes and black holes of Einstein gravity in $D=5$ space-time dimensions with multiple scalars and an arbitrary bulk potential. | contribution 0.83 | 0.94 | 0.07 | asserted 0.98 |
| s1 | As an application, we consider a thermodynamically unstable state of mass deformed ${\cal N}=4$ supersymmetric Yang-Mills theory at strong coupling. | contribution 0.88 | 0.46 | 0.05 | asserted 0.96 |
| s2 | The corresponding gravitational dual is ${\cal N}=2^*$ black brane with a dynamical instability of its translationary invariant horizon. | background 0.49 | 0.29 | 0.13 | asserted 1.00 |
| s3 | We study the dependence of the quasinormal mode spectra as the boundary gauge theory is compactified on $S^3$ -- the black brane is turned into the black hole. | contribution 0.90 | 0.87 | 0.07 | asserted 0.97 |
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The paper
Original abstract
We extend Kodama-Ishibashi and Jansen-Rostworowski-Rutkowski master field framework to study quasinormal modes of black branes and black holes of Einstein gravity in $D=5$ space-time dimensions with multiple scalars and an arbitrary bulk potential. As an application, we consider a thermodynamically unstable state of mass deformed ${\cal N}=4$ supersymmetric Yang-Mills theory at strong coupling. The corresponding gravitational dual is ${\cal N}=2^*$ black brane with a dynamical instability of its translationary invariant horizon. We study the dependence of the quasinormal mode spectra as the boundary gauge theory is compactified on $S^3$ -- the black brane is turned into the black hole.
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References
How the literature uses it
3 arXiv papers cite this in 15 sentences
Papers citing it · 6 sentences without a confident label
Uses its method or tool 2 papers
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Using the background parameterization [ref], we obtain from [ref] : [equation] where the second-order differential operator $_2$ (coming from $□$ on the background geometry [ref]) is (note that $k^2=K ℓ(ℓ+2)=0$) [equation] and [equation] with [equation]
Compactified holographic conformal order · $h=0$ QNMs of the hairy black holes in $𝔐_PW^b$ model · 0.93
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Linearized equations for gravity and scalar perturbations in different spin sectors are derived according to the master formula approach [ref] in the Eddington-Finkelstein coordinates.
Relativistic hydrodynamics with phase transition · Summary of main results and method · 1.00
What it cites · 51 sentences without a confident label
Builds on 6 papers
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In appendix [ref] we extend the QNM analysis of [ref] to black branes/holes in theories of Einstein gravity in $D=5$ space-time dimensions with multiple scalars and an arbitrary bulk potential: [equation] We then apply the general formalism to $=2^*$ holographic model [ref] , summarizing the results in section [ref].
N=1 Supersymmetric Renormalization Group Flows from IIB Supergravity · Introduction · 0.95
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In appendix [ref] we extend the QNM analysis of [ref] to black branes/holes in theories of Einstein gravity in $D=5$ space-time dimensions with multiple scalars and an arbitrary bulk potential: [equation] We then apply the general formalism to $=2^*$ holographic model [ref] , summarizing the results in section [ref].
Gauge Dual and Noncommutative Extension of an N=2 Supergravity Solution · Introduction · 0.95
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In appendix [ref] we extend the QNM analysis of [ref] to black branes/holes in theories of Einstein gravity in $D=5$ space-time dimensions with multiple scalars and an arbitrary bulk potential: [equation] We then apply the general formalism to $=2^*$ holographic model [ref] , summarizing the results in section [ref].
The Enhancon and N=2 Gauge Theory/Gravity RG Flows · Introduction · 0.95
Uses the method or tool of 3 papers
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The remaining fluctuations can be expressed through the master scalars [ref] as [equation] [equation] [equation] where $D$ is given by [ref], and $g$ is an arbitrary constant parameter of the unfixed gauge transformation [ref] .
Master equations and stability of Einstein-Maxwell-scalar black holes · $ℓ=1$ · 0.85
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We refer the reader to [ref] for a detailed discussion exactly how the gauge invariant fluctuations are constructed[In a holographic setting gauge invariant fluctuations in Einstein-scalar theories were used for the first time in [ref] .].
Sound waves in strongly coupled non-conformal gauge theory plasma · Master equations of Einstein-scalar black holes in $D=5$ · 0.80
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We add some practical remarks for the QNM computation. * In solving the QNM boundary value problems we use the shooting method developed in [ref] . * To obtain results for the QNMs reported in figs.
The black hole in the throat - thermodynamics of strongly coupled cascading gauge theories · Helicity $h=0$ QNMs of the PW black holes · 0.95
Uses data or values from 2 papers
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The unstable thermal state of interest once again is indicated with the purple dot — here the temperature $T_p$ is given by [ref], and the specific values of the transport coefficients are [equation] where we included the universal result for the shear viscosity $η$ as well [ref] .
Universality of the shear viscosity in supergravity · (A) · 0.93
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The unstable thermal state of interest once again is indicated with the purple dot — here the temperature $T_p$ is given by [ref], and the specific values of the transport coefficients are [equation] where we included the universal result for the shear viscosity $η$ as well [ref] .
Viscosity in Strongly Interacting Quantum Field Theories from Black Hole Physics · (A) · 0.93
Compares with 4 papers
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[ref] agrees with the results reported in [ref] , obtained using a completely different method. * While we did not present the AdS$_5$-Schwarzschild results for the $h=0$ sector graviton QNMs[See however [ref] .], obtained solving for the QNM spectrum from [ref] at $=1/100$, we confirmed that the results obtained are in agreement with $Δ=4$ results reported in [ref] , obtained using a completely different method. * We use the master field formalism [ref] , but we use finite difference rather than the spectral methods in computing the QNMs, as well as a different background geometry parameterization.
Master equations and stability of Einstein-Maxwell-scalar black holes · Numerical tests · 0.99
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[ref] agrees with the results reported in [ref] , obtained using a completely different method. * While we did not present the AdS$_5$-Schwarzschild results for the $h=0$ sector graviton QNMs[See however [ref] .], obtained solving for the QNM spectrum from [ref] at $=1/100$, we confirmed that the results obtained are in agreement with $Δ=4$ results reported in [ref] , obtained using a completely different method. * We use the master field formalism [ref] , but we use finite difference rather than the spectral methods in computing the QNMs, as well as a different background geometry parameterization.
AdS/CFT correspondence, quasinormal modes, and thermal correlators in N=4 SYM · Numerical tests · 0.99
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We recover[Our current numerical algorithms are more precise.] the previous results. * The hydrodynamics of $=2^*$ black brane was discussed earlier (again in a different parameterization) in [ref] .
Bulk viscosity of gauge theory plasma at strong coupling · Numerical tests · 0.96
Cites as support 4 papers
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The presence of such dynamical instability in thermodynamically unstable horizons was explicitly verified in [ref] .
A holographic perspective on Gubser-Mitra conjecture · Introduction · 0.98
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The presence of such dynamical instability in thermodynamically unstable horizons was explicitly verified in [ref] .
Bulk viscosity of N=2* plasma · Introduction · 0.98
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The presence of such dynamical instability in thermodynamically unstable horizons was explicitly verified in [ref] .
Critical phenomena in N=4 SYM plasma · Introduction · 0.98
Cites as background 14 papers
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In [ref] the authors formulated the correlated stability conjecture (CSC): A black brane thermodynamic (in)stability correlates with its dynamical (in)stability The conjecture is applicable only to horizons with translational invariance, simple higher-dimensional Schwarzschild black holes in Einstein gravity with a cosmological constant are stable [ref] .
Instability of charged black holes in anti-de Sitter space · Introduction · 0.84
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In [ref] the authors formulated the correlated stability conjecture (CSC): A black brane thermodynamic (in)stability correlates with its dynamical (in)stability The conjecture is applicable only to horizons with translational invariance, simple higher-dimensional Schwarzschild black holes in Einstein gravity with a cosmological constant are stable [ref] .
Stability of Higher-Dimensional Schwarzschild Black Holes · Introduction · 0.84
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In [ref] the authors formulated the correlated stability conjecture (CSC): A black brane thermodynamic (in)stability correlates with its dynamical (in)stability The conjecture is applicable only to horizons with translational invariance, simple higher-dimensional Schwarzschild black holes in Einstein gravity with a cosmological constant are stable [ref] .
The evolution of unstable black holes in anti-de Sitter space · Introduction · 0.84
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