The Kerr metric

Teukolsky, Saul A.

doi:10.1088/0264-9381/32/12/124006

Cited by 160 publications

(137 citation statements)

References 158 publications

(223 reference statements)

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“…For instance, studies like [34,43] identify the dominant source for the peak of the waveform during the plunge of a test particle into a Schwarzschild BH with the particle crossing the light ring. 7 Furthermore, the last few cycles of the BBH GW signal are associated with the dynamics of a linearly perturbed BH [44][45][46]. However, one needs to bear in mind that these studies are performed using linear perturbation theory where such localizations are better defined.…”

Section: Conceptual Challengesmentioning

confidence: 99%

On choosing the start time of binary black hole ringdowns

et al. 2018

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The final stage of a binary black hole merger is ringdown, in which the system is described by a Kerr black hole with quasinormal mode perturbations. It is far from straightforward to identify the time at which the ringdown begins. Yet determining this time is important for precision tests of the general theory of relativity that compare an observed signal with quasinormal mode descriptions of the ringdown, such as tests of the no-hair theorem. We present an algorithmic method to analyze the choice of ringdown start time in the observed waveform. This method is based on determining how close the strong field is to a Kerr black hole (Kerrness). Using numerical relativity simulations, we characterize the Kerrness of the strong-field region close to the black hole using a set of local, gauge-invariant geometric and algebraic conditions that measure local isometry to Kerr. We produce a map that associates each time in the gravitational waveform with a value of each of these Kerrness measures; this map is produced by following outgoing null characteristics from the strong and near-field regions to the wave zone. We perform this analysis on a numerical relativity simulation with parameters consistent with GW150914-the first gravitational-wave detection. We find that the choice of ringdown start time of 3 ms after merger used in the GW150914 study [B. P. Abbott et al. (Virgo Collaboration and LIGO Scientific Collaboration), Phys. Rev. Lett. 116, 221101 (2016).] to test general relativity corresponds to a high dimensionless perturbation amplitude of ∼7.5 × 10 −3 in the strong-field region. This suggests that in higher signal-to-noise detections, one would need to start analyzing the signal at a later time for studies that depend on the validity of black hole perturbation theory.

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Section: Conceptual Challengesmentioning

confidence: 99%

On choosing the start time of binary black hole ringdowns

et al. 2018

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“…Several authors addressed the problem of finding the metric for a rotating object (see [26,99] for a historical review and references); however the analytical solution for the gravitational field of an axisymmetric source remained elusive for many years.…”

Section: Rotating Black Holesmentioning

confidence: 99%

“…Some others [99] suggest that the problem is irrelevant from the physical point of view, due to the fact that there is no Birkhoff's theorem for the Kerr space-time. Nevertheless, some authors have proposed models for a possible Kerr source [42,47,79] however; the problem remains open.…”

Section: What Is the Source Of The Kerr Field?mentioning

confidence: 99%

Slowly rotating supercompact Schwarzschild stars

Posada¹

2017

Monthly Notices of the Royal Astronomical Society

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AcknowledgmentsI am grateful to the universe, for its harmony. The project is the study of integral and surface properties of slowly rotating homogeneous masses in the gravastar limit R → R s , where R s is the Schwarzschild radius. For this purpose we followed the perturbative method proposed by Hartle in 1967. In this model, the relativistic equations of structure for a slowly rotating star were derived at second order in the angular velocity Ω. An interesting, and educational, application of this model was investigated by Chandrasekhar and Miller. I am indebted to the Department of Physics andIn their approach, they solved numerically the structure equations of a homogeneous star (constant energy density) up to the Buchdahl bound (9/8)R s . Based on this work, our objective was to investigate the interesting region below the Buchdahl bound R s < R < (9/8)R s , which has not been studied previously in the literature.Our results were astonishing. We found that the surface properties and quadrupole mass moment approach the values corresponding to those of the Kerr metric when expanded at second order in angular momentum. This remarkable result provides a long sought solution to the problem of the source of rotation in the Kerr spacetime.iv

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“…One of the most cherished beliefs is that astrophysical BHs are described by the Kerr geometry, characterized by only two parameters, its mass M and angular momentum J = aM [2]. This belief is borne out of uniqueness results in GR, and the fact that the Kerr geometry is linearly and most likely nonlinearly stable [3,14] against massless fluctuations.…”

Section: Introductionmentioning

confidence: 99%

Cosmic censorship and parametrized spinning black-hole geometries

Cardoso

Queimada

2015

Gen Relativ Gravit

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The "cosmic censorship conjecture" asserts that all singularities arising from gravitational collapse are hidden within black holes. We investigate this conjecture in a setup of interest for tests of General Relativity: black hole solutions which are parametrically small deviations away from the Kerr solution. These solutions have an upper bound on rotation, beyond which a naked singularity is visible to outside observers. We study whether these (generic) spacetimes can be spun-up past extremality with point particles or accretion disks. Our results show that cosmic censorship is preserved for generic parameterizations. We also present examples of special geometries which can be spun-up past extremality.

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The Kerr metric

Cited by 160 publications

References 158 publications

On choosing the start time of binary black hole ringdowns

On choosing the start time of binary black hole ringdowns

Slowly rotating supercompact Schwarzschild stars

Cosmic censorship and parametrized spinning black-hole geometries

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