### Citations

527 |
A Stress tensor for Anti-de Sitter gravity, Commun.Math.Phys
- Balasubramanian, Kraus
- 1999
(Show Context)
Citation Context ...ctually, it is just the conformal class that needs to be fixed. 2 can define a boundary stress energy tensor Tµν from which one can compute conserved quantities associated with asymptotic symmetries3 =-=[2, 3]-=-. The best way to define Tµν is to introduce a set of coordinates that is well adapted to the expansion of the Einstein equations off the conformal boundary. Such coordinates were first introduced by ... |

453 |
Holographic reconstruction of spacetime and renormalization
- Haro, Solodukhin, et al.
(Show Context)
Citation Context ...ctually, it is just the conformal class that needs to be fixed. 2 can define a boundary stress energy tensor Tµν from which one can compute conserved quantities associated with asymptotic symmetries3 =-=[2, 3]-=-. The best way to define Tµν is to introduce a set of coordinates that is well adapted to the expansion of the Einstein equations off the conformal boundary. Such coordinates were first introduced by ... |

348 |
The Global Nonlinear Stability of the Minkowski Space
- Christodoulou, Klainerman
- 1993
(Show Context)
Citation Context ...ether AdS with this boundary condition is nonlinearly stable. The nonlinear stability of Minkowski spacetime and de Sitter spacetime (having constant positive curvature) was established some time ago =-=[5, 6]-=-. Given the current interest in gauge/gravity duality, it is important to determine whether a similar result is true for AdS. It is well known that AdS is stable at the linearized level. There is an i... |

274 | Breaking an Abelian gauge symmetry near a black hole horizon,”
- Gubser
- 2008
(Show Context)
Citation Context ...a dimension two charged operator O in the dual theory with source φ1 and expectation value φ2. Since we want this condensate to turn on without being sourced, we set φ1 = 0. As Gubser first suggested =-=[13]-=-, the above action has the property that (electrically) charged black holes become unstable at low temperatures to developing scalar hair. The reason is essentially that the effective mass of the scal... |

247 |
Conformal invariants, Élie Cartan et les Mathmatiques d’Aujourd’hui, Asterisque
- Fefferman, Graham
- 1985
(Show Context)
Citation Context ... a set of coordinates that is well adapted to the expansion of the Einstein equations off the conformal boundary. Such coordinates were first introduced by Fefferman and Graham in their seminal paper =-=[4]-=-, and take the following form ds2 = L2 z2 [ dz2 + gµν(z)dx µdxν ] , (1.4) where the boundary is now located at z = 0. In [4], the authors have further shown that Einstein’s equations ensure that gµν(z... |

176 |
Building a Holographic Superconductor,” Phys
- Hartnoll, Herzog, et al.
(Show Context)
Citation Context ...e graviton. The goal of this paper is to extend these results to the superconducting regime. We add a lattice in the form of a periodic potential to the simplest (original) holographic superconductor =-=[10, 11]-=- and compute the optical conductivity. We find that below Tc, in addition to the superfluid, there is a normal fluid component with the following properties • It has simple Drude behavior at low frequ... |

140 |
Universality and scaling in gravitational collapse of a massless scalar
- Choptuik
- 1993
(Show Context)
Citation Context ... amplitude A1, one forms a “zero mass black hole” which is really a naked singularity. This was first found in studies of spherically symmetric scalar field collapse in asymptotically flat spacetimes =-=[8, 9]-=-. In that case, initial scalar fields with A < A1 just scatter and go off to infinity leaving a globally nonsingular spacetime. In AdS, these waves reflect off infinity and return to the interior. It ... |

108 |
Stability of a Schwarzschild singularity, Phys
- Regge, Wheeler
- 1957
(Show Context)
Citation Context ...decompose perturbations according to how they transform under diffeomorphisms on the sphere. Normal modes of AdS4 then come in two distinct classes: vector and scalar type gravitational perturbations =-=[12, 13, 14, 15, 16, 17]-=-. Scalartype gravitational perturbations depend on three integers. Two of these, `s ≥ 2 and |ms| ≤ `s, label the usual scalar spherical harmonics. The remaining integer, ps ≥ 0, labels the number of n... |

90 |
On the existence of n-geodesically complete or future complete solutions of Einstein’s equations with smooth asymptotic structure
- Friedrich
- 1986
(Show Context)
Citation Context ...ether AdS with this boundary condition is nonlinearly stable. The nonlinear stability of Minkowski spacetime and de Sitter spacetime (having constant positive curvature) was established some time ago =-=[5, 6]-=-. Given the current interest in gauge/gravity duality, it is important to determine whether a similar result is true for AdS. It is well known that AdS is stable at the linearized level. There is an i... |

85 |
Starinets, “Minkowski space correlators
- Son, O
- 2002
(Show Context)
Citation Context ...e The resonance in the conductivity at ω/µ̄ ≈ 1.5 can be understood on the gravity side as arising from a quasinormal mode oscillation of the black hole, just like the example in [8]. As discussed in =-=[35]-=- quasinormal modes correspond to poles in retarded Green’s functions. We can determine the quasinormal mode frequency by fitting the conductivity to σ(ω) = GR(ω) iω = 1 iω a+ b(ω − ω0) ω − ω0 . (4.7) ... |

77 |
Extrema of mass, stationarity, and staticity, and solutions to the Einstein Yang-Mills equations,
- Sudarsky, Wald
- 1992
(Show Context)
Citation Context ...ial, µ(x, y). For convenience we will imagine that the x and y directions are periodically identified so the black holes have finite horizon area and mass. We follow the approach of Sudarsky and Wald =-=[40]-=-. As usual for a diffeomorphism invariant theory, the Hamiltonian is a linear combination of the constraints plus surface terms: H = ∫ Σ [NaCa +N aAa(DiE i)] + surface terms (A.1) where Na is the laps... |

74 |
Einstein equations and conformal structure: existence of antide Sitter-type space-times
- Friedrich
- 1995
(Show Context)
Citation Context ...f a finite cylinder with boundary S2 ×R and metric ds2bdy = −dt2 + L2(dθ2 + sin2 θdφ2) (1.3) To evolve asymptotically AdS initial data, one needs to specify boundary conditions at infinity. Friedrich =-=[1]-=- has shown that Einstein’s equation has a well posed initial value problem for various choices of boundary conditions. The standard one adopted by gauge/gravity duality is to fix the boundary metric.2... |

61 |
Dynamics in nonglobally hyperbolic static space-times.
- Ishibashi, Wald
- 2004
(Show Context)
Citation Context ...decompose perturbations according to how they transform under diffeomorphisms on the sphere. Normal modes of AdS4 then come in two distinct classes: vector and scalar type gravitational perturbations =-=[12, 13, 14, 15, 16, 17]-=-. Scalartype gravitational perturbations depend on three integers. Two of these, `s ≥ 2 and |ms| ≤ `s, label the usual scalar spherical harmonics. The remaining integer, ps ≥ 0, labels the number of n... |

49 |
The formation of black holes and singularities in spherically symmetric gravitational collapse
- Christodoulou
- 1991
(Show Context)
Citation Context ... amplitude A1, one forms a “zero mass black hole” which is really a naked singularity. This was first found in studies of spherically symmetric scalar field collapse in asymptotically flat spacetimes =-=[8, 9]-=-. In that case, initial scalar fields with A < A1 just scatter and go off to infinity leaving a globally nonsingular spacetime. In AdS, these waves reflect off infinity and return to the interior. It ... |

45 |
Gravitational field of a particle falling in a Schwarzschild geometry analyzed in tensor harmonics”, Phys
- Zerilli
- 1970
(Show Context)
Citation Context ...decompose perturbations according to how they transform under diffeomorphisms on the sphere. Normal modes of AdS4 then come in two distinct classes: vector and scalar type gravitational perturbations =-=[12, 13, 14, 15, 16, 17]-=-. Scalartype gravitational perturbations depend on three integers. Two of these, `s ≥ 2 and |ms| ≤ `s, label the usual scalar spherical harmonics. The remaining integer, ps ≥ 0, labels the number of n... |

43 |
On weakly turbulent instability of anti-de Sitter space
- Bizon, Rostworowski
(Show Context)
Citation Context ...nearly unstable. It appears that generically, small finite perturbations evolve to form black holes. This was first seen in a model of gravity coupled to a spherically symmetric massless scalar field =-=[7]-=-. In this case, the metric has no independent degrees of freedom and is completely determined by the scalar field. Given an initial profile φ = Aψ(r) for the scalar field, one can solve the Einstein c... |

35 | Holography without translational symmetry,” arXiv:1301.0537 - Vegh |

32 | Gauge gravity duality for d-wave superconductors: prospects and challenges
- Benini, Herzog, et al.
- 2010
(Show Context)
Citation Context ...Perhaps the main drawback of such an approach is that our current model describes an s-wave superconductor. We still do not have a satisfactory description of a d-wave holographic superconductor. See =-=[36]-=- for a description of some of the difficulties. We have presented results for the optical conductivity in the superconducting region for only one value of the lattice amplitude A0 = 2 and one value of... |

30 | A new approach to static numerical relativity, and its application to Kaluza-Klein black
- Headrick, Kitchen, et al.
(Show Context)
Citation Context ... temperature given by T ≡ G(1)/4pi = (6 − µ21)/8pi and H1,2, S1,2, F and ψ are six functions of x and z, that we determine using the numerical methods described in [1], which were first introduced in =-=[19]-=- and studied in great detail in [20]. When A0 = 0 the problem reduces to the original holographic superconductor [11]. It was shown there that there is a critical value of T/µ such that above this val... |

26 | Holographic quantum criticality from multi-trace deformations
- Faulkner, Horowitz, et al.
(Show Context)
Citation Context ...he original homogeneous holographic superconductor. So (5.1) cannot hold. To reproduce (5.1) one would have to fix a large A0 and vary Tc by other means, perhaps by adding a double trace perturbation =-=[39]-=-. Acknowledgements It is a pleasure to thank D. Tong for collaboration at an early stage of this project. We also thank N. Iqbal and the participants of the Simons Symposium on Quantum Entanglement: F... |

24 |
On the Nonlinear Stability of Asymptotically Anti-de Sitter Solutions
- Dias, Horowitz, et al.
(Show Context)
Citation Context ...any) resonances. There are modes with large angular momentum ` which are concentrated in the asymptotic region and have frequencies close to AdS, so there are approximate resonances. But one can show =-=[28]-=- that for large `, ω − ωAdS ∝ `−1/2 (3.8) A formal perturbation argument suggests that this difference is large enough to avoid triggering an instability [28]. This argument applies to all asymptotica... |

23 |
Effective potential for even parity Regge-Wheeler gravitational perturbation equations
- Zerilli
- 1970
(Show Context)
Citation Context |

22 | Ricci solitons, Ricci flow, and strongly coupled CFT
- Figueras, Lucietti, et al.
(Show Context)
Citation Context ... (6 − µ21)/8pi and H1,2, S1,2, F and ψ are six functions of x and z, that we determine using the numerical methods described in [1], which were first introduced in [19] and studied in great detail in =-=[20]-=-. When A0 = 0 the problem reduces to the original holographic superconductor [11]. It was shown there that there is a critical value of T/µ such that above this value, the scalar field vanishes and th... |

16 |
Further Evidence for
- Horowitz, Santos, et al.
(Show Context)
Citation Context ...avitational side is still not understood. It has been shown that a similar power-law is seen in the thermoelectric conductivity and for a 3 + 1 dimensional conductor 2 (although the exponents differ) =-=[8]-=-. In a recent paper, Vegh [9] studied the optical conductivity in a holographic model in which momentum conservation was broken by a graviton mass term. He finds a similar power-law scaling of the con... |

16 |
A gravity derivation of the Tisza-Landau Model
- Sonner, Withers
(Show Context)
Citation Context ...different holographic realization of a two fluid model, it was found that ρn remained nonzero at T = 0 when the charge on the scalar field was small, but vanished when the scalar charge became larger =-=[28]-=-. 12 0.0 0.2 0.4 0.6 0.8 1.0 0 20 40 60 80 100 120 140 TêTc t m Figure 7: The relaxation time as a function of temperature, extracted from the fit to (4.3). The dashed curve is a fit to (4.5). 4.2 Pow... |

15 |
Black holes with only one Killing field
- Dias, Horowitz, et al.
- 2011
(Show Context)
Citation Context ...ction for a rotating scalar field solution in AdS called a rotating boson star. In that case it has been shown that putting a small rotating black hole in the center does not destabilize the solution =-=[29]-=-. If rotating black holes do exist inside geons, it would clearly show that Kerr-AdS is not the only stationary, asymptotically AdS vacuum black hole. We conclude with some open questions raised by th... |

14 | Sum Rules from an Extra Dimension
- Gulotta, Herzog, et al.
(Show Context)
Citation Context ...deed approaches the superfluid density at large ω. At the end of the integration, they differ by less than 0.6%. This is not only a confirmation that our holographic superconductor satisfies the 7See =-=[31, 32, 33]-=- for general discussions of sum rules from gravity for translationally invariant backgrounds. 14 Figure 9: A log-log plot of the optical conductivity in eight BSCCO samples ranging from underdoped (UD... |

12 |
Visualizing pair formation on the atomic scale in the high-Tc superconductor Bi2Sr2CaCu2O8+δ,” Nature 447
- Gomes, Pasupathy, et al.
- 2007
(Show Context)
Citation Context ...ed red line on the right is a fit to (4.4). 11 excited quasiparticles with a gap ∆, but in BCS theory the gap is smaller, ∆ ≈ 1.7 Tc. Observations on the cuprates indeed show a gap of order ∆ = 4.0Tc =-=[26]-=-, showing that they are not weakly coupled superconductors. In the early work on holographic superconductors, an attempt was made to measure this gap. Since the system was homogeneous, there was no Dr... |

10 |
The quasi-normal modes of quantum criticality
- Witczak-Krempa, Sachdev
(Show Context)
Citation Context ...deed approaches the superfluid density at large ω. At the end of the integration, they differ by less than 0.6%. This is not only a confirmation that our holographic superconductor satisfies the 7See =-=[31, 32, 33]-=- for general discussions of sum rules from gravity for translationally invariant backgrounds. 14 Figure 9: A log-log plot of the optical conductivity in eight BSCCO samples ranging from underdoped (UD... |

10 |
AdS flowing black funnels: Stationary AdS black holes with non-Killing horizons and heat transport in the dual CFT, Class.Quant.Grav
- Fischetti, Marolf, et al.
(Show Context)
Citation Context ...ond condition is met in our case, the first is certainly not obvious. In fact, our system of equations appears to be of the mixed Elliptic-Hyperbolic type, for which the De-Turck method seems to work =-=[24, 25]-=-, even though we do not have a current understanding of why that is the case. In a nutshell, we are going to use Eq. (3.5), and a posteriori check that each of the components of ξ are zero to machine ... |

9 |
Inhomogeneous charged black hole solutions in asymptotically anti-de Sitter spacetime
- Maeda, Okamura, et al.
(Show Context)
Citation Context ... only introduced in one direction for computational convenience, and we will compute the conductivity only in the direction of the lattice. This “ionic” lattice has been discussed earlier (see, e.g., =-=[14, 15, 16, 17, 18]-=-) but almost always treated perturbatively. In [8] it was treated exactly in the theory (2.1) without the charged scalar field. Our model has several parameters. In principle one could vary the mass a... |

8 |
Stationary holographic plasma quenches and numerical methods for non-Killing horizons
- Figueras, Wiseman
(Show Context)
Citation Context ...ond condition is met in our case, the first is certainly not obvious. In fact, our system of equations appears to be of the mixed Elliptic-Hyperbolic type, for which the De-Turck method seems to work =-=[24, 25]-=-, even though we do not have a current understanding of why that is the case. In a nutshell, we are going to use Eq. (3.5), and a posteriori check that each of the components of ξ are zero to machine ... |

7 |
Quantum critical behaviour in a high-Tc superconductor,” Nature 425
- Marel, Molegraaf, et al.
- 2003
(Show Context)
Citation Context ...ependent phase of 60o. This difference is likely connected with the constant off-set in our power law. Without the offset, scale invariance, causality and time reversal symmetry require σ(ω) ∝ (−iω)α =-=[2]-=-, so the phase is related to the exponent of the power law. 4.3 Sum rule The Ferrell-Glover-Tinkham (FGT) sum rule states that the reduction in the spectral weight when T < Tc is taken up by the super... |

7 |
Generic instability of rotating relativistic stars
- Friedman
- 1978
(Show Context)
Citation Context ...he asymptotic region near the equator, indicates the presence of an ergoregion that extends all the way to the conformal boundary. This suggests a possible instability similar to the one discussed in =-=[27]-=-. If geons are linearly stable, they are likely to be nonlinearly stable as well. This is because there are very few (if any) resonances. There are modes with large angular momentum ` which are concen... |

6 |
Siopsis,“Enhancement of Critical Temperature of a Striped Holographic Superconductor”, Phys
- Ganguli, Hutasoit, et al.
- 2012
(Show Context)
Citation Context ...r critical temperature with charge). Comparing the different curves for a given charge, we see that increasing the lattice amplitude also increases the critical temperature. This was first noticed in =-=[21]-=- when the lattice was treated perturbatively. It can be understood as follows. As we said, the critical temperature of a uniform holographic superconductor is proportional to µ. By making µ vary perio... |

6 |
Renormalization group, secular term resummation and AdS (in)stability,
- Craps, Evnin, et al.
- 2014
(Show Context)
Citation Context ...ging the boundary conditions for a massless scalar field, or by adding a mass one can remove the resonances in the linear spectrum. Some 5For example, our resonant mode matches the general results of =-=[18]-=- for the scalar case. 6 numerical evolutions show that black holes form only when the linear spectrum has resonances [19], while other authors [20] find that collapse always occurs, even when the line... |

5 |
Towards a Holographic Realization
- Erdmenger, Kerner, et al.
(Show Context)
Citation Context ...e also choose Na = (∂/∂t)a. Now under a perturbation of the black hole δH = ∫ δqij∂H/∂qij + · · · = 0 (A.3) 8An earlier unsuccessful attempt to find a holographic realization of Homes law was made in =-=[38]-=-. 18 since the partial derivatives of the Hamiltonian just yield the time derivatives of the canonical variables in the background which vanish since the background is static. On the other hand, if th... |

5 |
Holographic Thermalization, stability of AdS, and the Fermi-Pasta-Ulam-Tsingou paradox
- Balasubramanian, Buchel, et al.
(Show Context)
Citation Context ... collapse always occurs, even when the linear spectrum is not resonant. If this is correct, there must be another explanation for the instability. Another numerical evolution of two mode initial data =-=[21]-=- did not find an instability. One difficulty with numerical evolutions is that they only last a finite time. Since the timescale for the instability is expected to grow like 1/2, one cannot probe arb... |

4 | Scaling properties of the optical conductivity of Bi-based cuprates,” Annals of Physics 321
- Marel, Carbone, et al.
- 2006
(Show Context)
Citation Context ...ttice spacing, lattice amplitude, and temperature. Strikingly, a power-law at mid-infrared frequencies with exactly this exponent is seen in measurements of the normal phase of bismuth-based cuprates =-=[2, 3]-=-. (See also [4] for earlier experimental results and [5, 6, 7] for attempts to explain this scaling). Also in agreement with the measurements is the fact that the coefficient B is temperature independ... |

4 |
Infrared Conductivity of Cuprate Metals: Detailed Fit Using LuttingerLiquid Theory”, Phys
- Anderson
- 1997
(Show Context)
Citation Context ...ly, a power-law at mid-infrared frequencies with exactly this exponent is seen in measurements of the normal phase of bismuth-based cuprates [2, 3]. (See also [4] for earlier experimental results and =-=[5, 6, 7]-=- for attempts to explain this scaling). Also in agreement with the measurements is the fact that the coefficient B is temperature independent, although the cuprates do not appear to have the off-set C... |

4 |
A Striped Holographic
- Flauger, Pajer, et al.
(Show Context)
Citation Context ... only introduced in one direction for computational convenience, and we will compute the conductivity only in the direction of the lattice. This “ionic” lattice has been discussed earlier (see, e.g., =-=[14, 15, 16, 17, 18]-=-) but almost always treated perturbatively. In [8] it was treated exactly in the theory (2.1) without the charged scalar field. Our model has several parameters. In principle one could vary the mass a... |

4 |
Dispersing quasinormal modes in 2+1 dimensional conformal field theories, Phys.Rev. B87
- Witczak-Krempa, Sachdev
- 2013
(Show Context)
Citation Context ...deed approaches the superfluid density at large ω. At the end of the integration, they differ by less than 0.6%. This is not only a confirmation that our holographic superconductor satisfies the 7See =-=[31, 32, 33]-=- for general discussions of sum rules from gravity for translationally invariant backgrounds. 14 Figure 9: A log-log plot of the optical conductivity in eight BSCCO samples ranging from underdoped (UD... |

4 |
Time-Periodic Solutions in an Einstein AdS-Massless-Scalar-Field System,
- Maliborski, Rostworowski
- 2013
(Show Context)
Citation Context ...le mode of the scalar field, there 4 appeared to be no problem adding higher order corrections and keeping the solution time periodic. Indeed these “oscillons” have since been constructed numerically =-=[10]-=-. They represent exact, time periodic, spherically symmetric solutions of the Einstein-scalar field equations. Since this model is spherically symmetric, no gravitational degrees of freedom are excite... |

4 |
On the nonlinear instability of confined geometries,” arXiv:1409.0533 [gr-qc
- Okawa, Cardoso, et al.
(Show Context)
Citation Context ...le, our resonant mode matches the general results of [18] for the scalar case. 6 numerical evolutions show that black holes form only when the linear spectrum has resonances [19], while other authors =-=[20]-=- find that collapse always occurs, even when the linear spectrum is not resonant. If this is correct, there must be another explanation for the instability. Another numerical evolution of two mode ini... |

3 |
Thermodynamics and Optical Conductivity of a Dissipative Carrier in a Tight Binding
- Kato, Imada
- 1998
(Show Context)
Citation Context ...ly, a power-law at mid-infrared frequencies with exactly this exponent is seen in measurements of the normal phase of bismuth-based cuprates [2, 3]. (See also [4] for earlier experimental results and =-=[5, 6, 7]-=- for attempts to explain this scaling). Also in agreement with the measurements is the fact that the coefficient B is temperature independent, although the cuprates do not appear to have the off-set C... |

3 | Gu,”Doping dependent optical properties of Bi2Sr2CaCu2O8
- Hwang, Timusk, et al.
- 2007
(Show Context)
Citation Context ...of the bismuth-based cuprates. In particular, experiments have shown that the power-law is unchanged when the temperature drops below the critical temperature and the material becomes superconducting =-=[12]-=-. 2 Gravitational model We will work with the simplest holographic superconductor which requires gravity coupled to a Maxwell field and charged scalar Φ. The action is S = 1 16piGN ∫ d4x √−g [ R + 6 L... |

3 | Striped superconductors: How the cuprates intertwine spin, charge and superconducting orders
- Berg, Fradkin, et al.
(Show Context)
Citation Context ...a solution in which Φ changes sign from one region of size λ0 to the next, by simply starting with a seed solution in 2It is not a gravitational dual of the novel striped superconductor introduced in =-=[23]-=- since that required a condensate whose average value was zero. 8 Newton’s iterative method that changes sign. Given this, one can construct solutions with period (n + m)λ0 in which Φ changes sign on ... |

2 |
Microwave determination of the quasiparticle scattering time in YBa2Cu3O6.95.
- Bonn
- 1993
(Show Context)
Citation Context ...d line in Fig. 7 is a fit to τ = τ0 e ∆̃/T with ∆̃ = 4.3 Tc . (4.5) It follows that the scattering rate, 1/τ , drops rapidly as T is reduced below Tc. This is another observed feature of the cuprates =-=[30]-=-. One often distinguishes clean and dirty limits of superconductors by comparing the scattering rate to the gap. It is easy to check that our holographic superconductor is in the clean limit: 1/τ 2∆... |

2 |
Decay properties of Klein-Gordon fields
- Holzegel, Smulevici
(Show Context)
Citation Context ...ntially in time. However, it has been shown that perturbations of AdS black holes with finite Sobelov norm only decay like 1/(log t)p where the exponent depends on which Sobelov space one starts with =-=[30]-=-. Even analytic perturbations typically fall-off only as a power of 1/t. This slow decay might indicate an instability. On the other hand, perturbative 12 arguments based on resonances indicate that A... |

1 |
Chubukov, High-frequency behavior of the infrared conductivity of cuprates, Phys
- Norman, V
(Show Context)
Citation Context ...ly, a power-law at mid-infrared frequencies with exactly this exponent is seen in measurements of the normal phase of bismuth-based cuprates [2, 3]. (See also [4] for earlier experimental results and =-=[5, 6, 7]-=- for attempts to explain this scaling). Also in agreement with the measurements is the fact that the coefficient B is temperature independent, although the cuprates do not appear to have the off-set C... |

1 |
Optical Conductivity and spatial inhomogeneity in cuprate superconductors, in Handbook of high-temperature superconductivity. Theory and experiment
- Orenstein
- 2007
(Show Context)
Citation Context ...f we believe this extrapolation then ρn remains nonzero even at zero temperature indicating uncondensed spectral weight.5 Observations on the cuprates indeed show uncondensed spectral weight at T = 0 =-=[29]-=-. Of course the cuprates are d-wave superconductors in which the gap has nodes on the Fermi surface which probably contribute to this effect. It is surprising to see ρn 6= 0 at T = 0 in an s-wave supe... |

1 |
Scaling of the superfluid density in high-temperature superconductors
- Homes, Dordevic, et al.
- 2005
(Show Context)
Citation Context ...ular horizon. Homes has discovered a remarkable relation between the low temperature superfluid density ρs, the critical temperature Tc and the DC conductivity just above the critical temperature σdc =-=[37]-=-. He found that for a wide range of high temperature superconductors ρs ≈ 35σdc Tc . (5.1) This relation appears to be universal. It holds for the conductivity perpendicular to the CuO2 planes in the ... |

1 |
Differential equations for perturbations on the schwarzschild metric, Phys.Rev. D1
- Edelstein, Vishveshwara
- 1970
(Show Context)
Citation Context |

1 |
Stability of the schwarzschild metric, Phys.Rev. D1
- Vishveshwara
- 1970
(Show Context)
Citation Context |

1 |
What drives AdS unstable?, Phys.Rev. D89
- Maliborski, Rostworowski
- 2014
(Show Context)
Citation Context ... spectrum. Some 5For example, our resonant mode matches the general results of [18] for the scalar case. 6 numerical evolutions show that black holes form only when the linear spectrum has resonances =-=[19]-=-, while other authors [20] find that collapse always occurs, even when the linear spectrum is not resonant. If this is correct, there must be another explanation for the instability. Another numerical... |