Black-hole microstate spectroscopy: Ringdown, quasinormal modes, and echoes

Self Cite

We exploit the recently proposed correspondence between gravitational perturbations and quantum Seiberg-Witten curves to compute the spectrum of quasi-normal modes of asymptotically flat Kerr Newman black holes and establish detailed gauge/gravity dictionaries for a large class of black holes, D-branes and fuzzballs in diverse dimensions. QNM frequencies obtained from the quantum periods of SU(2) $$ \mathcal{N} $$ N = 2 SYM with Nf = 3 flavours are compared against numerical results, WKB (eikonal) approximation and geodetic motion showing remarkable agreement. Starting from the master example relating quasi-normal modes of Kerr-Newman black holes in AdS4 to SU(2) gauge theory with Nf = 4, we illustrate the procedure for some simple toy-models that allow analytic solutions. We also argue that the AGT version of the gauge/gravity correspondence may give precious hints as to the physical/geometric origin of the quasi-normal modes/Seiberg-Witten connection and further elucidate interesting properties (such as tidal Love numbers and grey-body factors) that can help discriminating black holes from fuzzballs.

“…λ is known as the Lyapunov exponent and quantifies the chaotic behavior of nearly critical geodesics around the photon-sphere [2,[6][7][8][9]. We write…”

Section: Geodetic Motionmentioning

confidence: 99%

Section: Numerical Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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More on the SW-QNM correspondence

Bianchi

Consoli

Grillo

et al. 2022

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“…Recent studies of supersymmetric microstate geometries include the analysis of their shadows and images [57] (relevant for EHT observations), and scalar field echoes on these geometries [58] (relevant for the ringdown phase in mergers). These studies showed the intricate and subtle behavior that allows the supersymmetric microstate geometries to behave very similarly to a black hole, but nevertheless allowing for certain observable signatures when far from the scaling point.…”

Section: Jhep10(2021)138 5 Conclusionmentioning

confidence: 99%

Gravitational footprints of black holes and their microstate geometries

Bah

Bena

Heidmann

et al. 2021

We construct a family of non-supersymmetric extremal black holes and their horizonless microstate geometries in four dimensions. The black holes can have finite angular momentum and an arbitrary charge-to-mass ratio, unlike their supersymmetric cousins. These features make them and their microstate geometries astrophysically relevant. Thus, they provide interesting prototypes to study deviations from Kerr solutions caused by new horizon-scale physics. In this paper, we compute the gravitational multipole structure of these solutions and compare them to Kerr black holes. The multipoles of the black hole differ significantly from Kerr as they depend non-trivially on the charge-to-mass ratio. The horizonless microstate geometries (that are comparable in size to a black hole) have a similar multipole structure as their corresponding black hole, with deviations to the black hole multipole values set by the scale of their microstructure.

“…such possible α corrections on radiation energy flux predicted by string theory in BH mergings dubbed string memory effect [35][36][37][38].…”

Section: Jhep11(2021)193mentioning

confidence: 99%

Soft gravitational radiation from multi-body collisions

Addazi

Zeng

2021

We derive a universal expression for the gravitational radiation energy spectrum dEGW/dω at sub-leading order emitted from a generic gravitational hard scattering of multi-particles or multi-bodies. Our result includes all $$ \mathcal{O} $$ O (ω) corrections to the gravitational radiation flux from a generic 2 → N collision, in both the cases of massless and massive particles/bodies. We also show the dependence of the radiation energy flux by the quantum spin in case of particle collisions. Then, we consider the specific case of a gravitational elastic scattering of two massive bodies, i.e. m + M → m + M with m, M the masses of the two bodies respectively. We demonstrate that in this case all $$ \mathcal{O} $$ O (ω) contributions to the energy flux exactly cancel each others. Nevertheless, we also show that, for a 2 → 2 inelastic scattering, the inclusion of sub-leading soft gravitons leads to a not zero radiation flux, having a simple expression in certain asymptotic regimes. Our results can be applied to the case of Black Hole collisions with possible testable implications in gravitational waves physics.