Constraining the Konoplya-Rezzolla-Zhidenko deformation parameters III: Limits from stellar-mass black holes using gravitational-wave observations

Swarnim, Shashank,; Bambi, Cosimo

doi:10.1103/physrevd.105.104004

Cited by 25 publications

(14 citation statements)

References 48 publications

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“…The essence of this approach is a general parametrization of the black-hole spacetime, similar in spirit with the post-Newtonian parametrized formalism, but working in the whole space outside the black hole including the nearhorizon zone. This formalism was extensively applied for analytic approximations of various numerical black-hole metrics (see, for instance, [22][23][24] and references therein) as well as for analysis of various radiation phenomena around them [25][26][27][28][29][30][31][32][33][34]. The advantage of this method is that frequently it allows one to approximate the black hole spacetime by only a few parameters for description of astrophysically relevant phenomena [35].…”

Section: General Parametrized Spherically Symmetric Black Hole In Ads...mentioning

confidence: 99%

Quasinormal ringing of regular black holes in asymptotically safe gravity: the importance of overtones

Konoplya

Zinhailo

Kunz

et al. 2022

J. Cosmol. Astropart. Phys.

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Asymptotically safe gravity is based on the idea that the main contribution to the Schwarzschild-like black hole spacetime is due to the value of the gravitational coupling which depends on the distance from the origin and approaches its classical value in the far zone. However, at some stage this approach has an arbitrariness of choice of some identification parameter. The two cases of identification are considered here: first, by the modified proper length (the Bonanno-Reuter metric), and second, by the Kretschmann scalar (the metric for this case coincides, up to the redefinition of constants, with the Hayward metric). Even though the quasinormal modes of these metrics have been extensively studied, a number of interesting points were missed. We have found that quasinormal modes are qualitatively similar for both types of identification. The deviation of the fundamental mode from its Schwarzschild limit may be a few times larger than it was claimed in the previous studies. The striking deviation from the Schwarzschild limit occurs for overtones, being as large as hundreds of percent even when the fundamental mode is almost coinciding with the Schwarzschild one. This happens because the above metrics are very close to the Schwarzschild one everywhere, except a small region near the event horizon, which is crucial for overtones. The spectrum of both metrics contains purely imaginary (non-oscillatory) modes, which, for some values of parameters, can appear already at the second overtone.

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Section: General Parametrized Spherically Symmetric Black Hole In Ads...mentioning

confidence: 99%

Quasinormal ringing of regular black holes in asymptotically safe gravity: the importance of overtones

Konoplya

Zinhailo

Kunz

et al. 2022

J. Cosmol. Astropart. Phys.

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“…We could certainly constrain q from the available gravitational wave data from the LIGO-Virgo-KAGRA Collaboration following the approach employed in Refs. [19,20] for testing other non-Kerr metrics. The deformation parameter q may also be constrained from the available mm black hole images from the Event Horizon Telescope Collaboration (see, e.g., Ref.…”

Section: Discussionmentioning

confidence: 99%

“…For both object classes, we have even a body of observations suggesting that these objects do not have a normal surface but an event horizon [14,15]. The past few years have seen a tremendous progress in our capability of testing the nature of these compact objects and today we can use gravitational wave data from the LIGO-Virgo-KAGRA Collaboration [16][17][18][19][20], X-ray observations from a number of X-ray missions [21][22][23][24][25][26][27], and the mm images of the supermassive objects in M87 * and Sgr A * from the Event Horizon Telescope Collaboration [28][29][30][31][32][33].…”

Section: Introductionmentioning

confidence: 99%

Testing the $δ$-Kerr metric with black hole X-ray data

Tao¹,

Riaz²,

Zhou³

et al. 2023

Preprint

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The spacetime around astrophysical black holes is thought to be described by the Kerr solution. However, even within general relativity, there is not yet a proof that the final product of the complete collapse of an uncharged body can only be a Kerr black hole. We can thus speculate on the possibility that the spacetime around astrophysical black holes may be described by other solutions of the Einstein Equations and we can test such a hypothesis with observations. In this work, we consider the δ-Kerr metric, which is an exact solution of the field equations in vacuum and can be obtained from a non-linear superposition of the Kerr metric with a static axially symmetric solution, often referred to as the δ-metric. The parameter δ = 1 + q quantifies the departure of the source from the Kerr metric and for q = 0 we recover the Kerr solution. From the analysis of the reflection features in the X-ray spectrum of the Galactic black hole in EXO 1846-031, we find −0.1 < q < 0.7 (90% CL), which is consistent with the hypothesis that the spacetime around the compact object in EXO 1846-031 is a Kerr black hole but does not entirely rule out the δ-Kerr metric.

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“…They provided models to account for astrophysical uncertainties linked to parameters in the accretion disk, and placed constraints on parameters characterizing circular deviations from Kerr, accounting for astrophysical uncertainties linked to parameters of the accretion disk. Another approach has been taken in [86,87], where constraints on deviation parameters were derived using gravitational wave data from the LIGO/VIRGO collaboration on the inspiral phase of black-hole mergers. Going forward, both approaches may be useful.…”

Section: Discussionmentioning

confidence: 99%

Parameterizations of black-hole spacetimes beyond circularity

Delaporte¹,

Eichhorn²,

Held³

2022

Class. Quantum Grav.

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We discuss parameterizations of black-hole spacetimes in and beyond General Relativity in view of their symmetry constraints: within the class of axisymmetric, stationary spacetimes, we propose a parameterization that includes non-circular spacetimes, both in Boyer-Lindquist as well as in horizon-penetrating coordinates. We show how existing parameterizations, which make additional symmetry assumptions (ﬁrst, circularity; second, a hidden constant of motion), are included in the new parameterization. Further, we explain why horizon-penetrating coordinates may be more suitable to parameterize non-circular deviations from the Kerr geometry. Our investigation is motivated by our result that the regular, spinning black-hole spacetimes proposed in [1, 2] are non-circular. This particular deviation from circularity can result in cusps, a dent and an asymmetry in the photon rings surrounding the black-hole shadow. Finally, we explore a new class of non-circular deviations from Kerr black holes, which promote the spin parameter to a function, and ﬁnd indications that regularity cannot be achieved in this setting. This result strengthens the case for regular black holes based on a promotion of the mass parameter to a function.

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Constraining the Konoplya-Rezzolla-Zhidenko deformation parameters III: Limits from stellar-mass black holes using gravitational-wave observations

Cited by 25 publications

References 48 publications

Quasinormal ringing of regular black holes in asymptotically safe gravity: the importance of overtones

Quasinormal ringing of regular black holes in asymptotically safe gravity: the importance of overtones

Testing the $δ$-Kerr metric with black hole X-ray data

Parameterizations of black-hole spacetimes beyond circularity

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