Testing the No-Hair Theorem with GW150914

Isi, M.; Giesler, Matthew; Farr, W. M.; Scheel, Mark A.; Teukolsky, Saul A.

doi:10.1103/physrevlett.123.111102

Cited by 382 publications

(419 citation statements)

References 71 publications

Supporting

Mentioning

395

Contrasting

Unclassified

Order By: Relevance

“…Such tests include observations of pulsar-BH binaries [7][8][9], the orbits of SMBH stellar companions [10][11][12], the electromagnetic accretion flows of SMBHs (continuume spectrum, iron lines, quasi-periodic oscillations, etc.) [13][14][15][16][17][18][19][20][21][22][23][24][25][26][27], the quasinormal ringdown modes of a post-coalescence perturbed remnant BH [28][29][30], and even the gravitational wave observations of extreme mass-ratio inspirals of super-massive and stellar-mass BHs [5,[31][32][33][34][35][36][37][38][39][40][41][42][43][44][45][46]. No significant deviations from the Kerr result have been detected so far.…”

Section: Introductionmentioning

confidence: 97%

Asymptotically flat, parametrized black hole metric preserving Kerr symmetries

Carson¹,

Yagi²

2020

Phys. Rev. D

View full text Add to dashboard Cite

Recently the Event Horizon Telescope Collaboration, with very-long baseline interferometric observations, resolved structure at the scale of ∼ 5 Schwarzschild radii about the center of M87 * , the supermassive black hole resident at the center of Messier 87. This important observation has paved the way for testing what is known as the "no-hair" theorem, stating that isolated black holes are described by the Kerr metric, parameterized only by their mass and spin. Generic, parameterized spacetimes beyond Kerr allow one to arbitrarily test the no-hair theorem for deviations from the Kerr result with no prior theoretical knowledge or motivation. In this paper, we present such a new general, stationary, axisymmetric and asymptotically flat black hole solution with separable geodesic equations (thus preserving symmetries of a Kerr black hole), extending the previous work of Johannsen. In this new metric, five free non-linear functions parameterically deviate from the Kerr result, allowing one to effectively transform to many alternative black hole solutions present in the literature. We then derive analytic expressions for the Keplerian and epicyclic frequencies, the orbital energy and angular momentum, and the location of the innermost stable orbit of circular equatorial particle orbits. We also compute the image of the photon rings in the new spacetime, which correspond to the boundary of the black hole shadow image taken by the Event Horizon Telescope. We finally compare each quantity for the Kerr result against various parameterizations of the metric, finding that, especially for highly rotating black holes, the two solutions disagree significantly. Such a metric parameterization allows one to perform the no-hair tests in a modelindependent way, and finally map constraints to specific alternative theories of gravity.

show abstract

Section: Introductionmentioning

confidence: 97%

Asymptotically flat, parametrized black hole metric preserving Kerr symmetries

Carson¹,

Yagi²

2020

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…[63][64][65][66][67]) for the remnant mass and spin to obtain posterior distributions for these quantities. Finally, considering only the ringdown signal and varying the quasi-normalmode frequencies [68][69][70][71], the remnant mass and spin are independently measured [16,19,21,22,73,74].…”

Section: A Implications For Tests Of General Relativitymentioning

confidence: 99%

“…The end state of the remnant is entirely characterized by its mass (m f ), spin (χ f ) and kick velocity (v f ); all additional complexities ("hair") [14,15] are dissipated away in GWs during the ringdown stage that follows the merger. The remnant mass and spin have already been measured from GW signals and used to test general relativity [16][17][18][19][20][21][22][23]. However, a measurement of the kick has remained elusive.…”

mentioning

confidence: 99%

Extracting the Gravitational Recoil from Black Hole Merger Signals

2020

Self Cite

View full text Add to dashboard Cite

Gravitational waves carry energy, angular momentum, and linear momentum. In generic binary black hole mergers, the loss of linear momentum imparts a recoil velocity, or a "kick", to the remnant black hole. We exploit recent advances in gravitational waveform and remnant black hole modeling to extract information about the kick from the gravitational wave signal. Kick measurements such as these are astrophysically valuable, enabling independent constraints on the rate of second-generation mergers. Further, we show that kicks must be factored into future ringdown tests of general relativity with third-generation gravitational wave detectors to avoid systematic biases. We find that, although little information can be gained about the kick for existing gravitational wave events, interesting measurements will soon become possible as detectors improve. We show that, once LIGO and Virgo reach their design sensitivities, we will reliably extract the kick velocity for generically precessing binaries-including the so-called superkicks, reaching up to 5000 km/s.

show abstract

“…One can extract the authentic values of these physical quantities from the observational data by the LIGO/VIRGO collaboration, see [1,2,13] and references therein.…”

Section: B the Schwarzschild Singularity In The Regge-wheeler And Zimentioning

confidence: 99%

“…For example, in GW from binary BH merger: "Rather than nonlinearities, times around the peak are dominated by ringdown overtones -the quasinormal modes with the fastest decay rates, but also the highest amplitudes near the waveform peak. ", see the very recent paper [13], and the references therein.…”

Section: B the Schwarzschild Singularity In The Regge-wheeler And Zimentioning

confidence: 99%

The Era of Gravitational Astronomy and Gravitational Field of Non-Rotating Single Point Particle in General Relativity

Fiziev

2019

Phys. Part. Nuclei

View full text Add to dashboard Cite

Utilizing various gauges of the radial coordinate, we give a General Relativistic (GR) description of static spherically symmetric spacetimes with a massive point source and vacuum outside this singularity. We show that in GR there exists a two-parameter family of such solutions to the Einstein equations which are physically distinguishable and describe the gravitational field of a single massive point particle with positive proper mass M0 and positive Keplerian mass M < M0. In particular, we show that the widespread Hilbert form of the Schwarzschild solution, which depends only on the Keplerian mass M and describes Black Holes (BH), does not solve the Einstein equations with a massive point particle stress-energy tensor. Novel normal coordinates for the gravitational field and a new physical class of gauges are proposed, thus achieving a correct description of a point mass source in GR. We also introduce a gravitational mass defect of a point particle and determine the dependence of the solutions on this mass defect. The result can be described as a change of the Newton potential ϕ N = −G N M/r to a modified one ϕ G = −G N M/ r + G N M/c 2 ln M 0 M and the corresponding modification of the four-interval. We show that the proper 3D flat space, where these two potentials can be compared, is the tangent space above the position of the massive point source. In addition, we present invariant characteristics of the physically and geometrically different classes of spherically symmetric static spacetimes created by a point mass. Our findings are important for description of Extremely Compact Objects (ECOs) studied in relation with possible echoes in Gravitational Waves (GW) recently discovered by the LIGO/VIRGO collaboration.The used methods also turned out to be not enough to establish the existence or absence of echoes as fingerprints of Extremely Compact Objects (ECOs) 1 , which are not BH [14][15][16][17][18][19][20].Between others, GW150914 is the event with the largest signal-to-noise-ratio in the QNMs ringing domain. None of the methods, recently proposed for finding echoes, have yet found a significant echo signal in this event [17] or discarded firmly their existence.As a result, we still cannot refute firmly many of the alternative theoretical explanations for the sources of GW events observed by the LIGO/VIRGO collaboration.For recent reviews on the above problems, as well as on a series of other ones, see the talk by Alan Weinstein at the First LIGO Open Data Workshop 2018 [1] and a large review paper on the general situation in gravity [2].The most recent observation of the shadow of the ECO at the center of the elliptic galaxy M87 proves the extremal compact character of the central object [21] but it does not give any indication of the presence or absence of an event horizon of this object.In the present paper, we consider in a mathematically correct way the most compact object -a non-rotating massive point particle in GR.We dub this subject "the Schwarzschild problem", since the first attempt to solve i...

show abstract

Testing the No-Hair Theorem with GW150914

Cited by 382 publications

References 71 publications

Asymptotically flat, parametrized black hole metric preserving Kerr symmetries

Asymptotically flat, parametrized black hole metric preserving Kerr symmetries

Extracting the Gravitational Recoil from Black Hole Merger Signals

The Era of Gravitational Astronomy and Gravitational Field of Non-Rotating Single Point Particle in General Relativity

Contact Info

Product

Resources

About