Gravitational radiation close to a black hole horizon: Waveform regularization and the out-going echo

Srivastava, Manu; Chen, Yanbei

doi:10.1103/physrevd.104.104006

Cited by 7 publications

(5 citation statements)

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“…where h + and h × are two GW polarizations that encode the information of GW strain, ∂ 2 t denotes the double partial derivative with respect to time. Further, the Teukolsky equation in terms of various NP quantities and different operators are written in the following form [71,77,78],…”

Section: Jcap01(2023)046mentioning

confidence: 99%

Gravitational wave from extreme mass-ratio inspirals as a probe of extra dimensions

Rahman

Kumar

Bhattacharyya

2023

J. Cosmol. Astropart. Phys.

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The field of gravitational waves is rapidly progressing due to the noticeable advancements in the sensitivity of gravitational-wave detectors that has enabled the detection prospects of binary black hole mergers. Extreme mass-ratio inspiral (EMRI) is one of the most compelling and captivating binary systems in this direction, with the detection possibility by the future space-based gravitational wave detector. In this article, we consider an EMRI system where the primary or the central object is a spherically symmetric static braneworld black hole that carries a tidal charge Q. We estimate the effect of the tidal charge on total gravitational wave flux and orbital phase due to a non-spinning secondary inspiralling the primary. We further highlight the observational implications of the tidal charge in EMRI waveforms. We show that LISA (Laser Interferometer Space Antenna) observations can put a much stronger constraint on this parameter than black hole shadow and ground-based gravitational wave observations, which can potentially probe the existence of extra dimensions.

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Section: Jcap01(2023)046mentioning

confidence: 99%

Gravitational wave from extreme mass-ratio inspirals as a probe of extra dimensions

Rahman

Kumar

Bhattacharyya

2023

J. Cosmol. Astropart. Phys.

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“…Working on a sourceless system, Nakano et al [54] imposed a complete reflecting boundary condition at a constant Boyer-Lindquist radius. Later, the effect of source terms was investigated [55][56][57][58][59][60]. Sago and Tanaka [55] and Maggio et al [56] studied main GWs and echoes generated by a particle that plunges into a Kerr black hole.…”

Section: Introductionmentioning

confidence: 99%

“…[57]. References [58][59][60] further introduced the backreaction of GW emissions on orbital motion.…”

Section: Introductionmentioning

confidence: 99%

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Gravitational-wave echoes from numerical-relativity waveforms via spacetime construction near merging compact objects

Wang

Deppe

et al. 2022

Phys. Rev. D

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We propose a new approach toward reconstructing the late-time near-horizon geometry of merging binary black holes, and toward computing gravitational-wave echoes from exotic compact objects. A binary black-hole merger spacetime can be divided by a timelike hypersurface into a black-hole perturbation (BHP) region (in which the spacetime geometry can be approximated by homogeneous linear perturbations of the final Kerr black hole) and a nonlinear region. At late times, the boundary between the two regions is an infalling shell. The BHP region contains late-time gravitational waves emitted toward the future horizon, as well as those emitted toward future null infinity. In this region, by imposing no-ingoing-wave conditions at past null infinity and matching outgoing waves at future null infinity with waveforms computed from numerical relativity, we can obtain waves that travel toward the future horizon. In particular, the Newman-Penrose ψ 0 associated with the ingoing wave on the horizon is related to tidal deformations measured by fiducial observers floating above the horizon. We further determine the boundary of the BHP region on the future horizon by imposing that ψ 0 inside the BHP region can be faithfully represented by quasinormal modes. Using a physically motivated method to impose boundary conditions near the horizon and applying the so-called Boltzmann reflectivity, we compute the quasinormal modes of nonrotating exotic compact objects, as well as gravitational-wave echoes. We also investigate the detectability of these echoes in current and future detectors and prospects for parameter estimation.

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“…Several tests have been proposed to probe whether the compact objects in a binary are BHs or ECOs. One of them is using echoes to distinguish the remnants of binary merger from BHs, which has initiated rigorous modeling and the search for those features in GW data [12,[20][21][22][23][24][25][26][27][28][29][30][31][32]. The construction of waveforms for binary ECOs has also begun [33,34].…”

Section: Introductionmentioning

confidence: 99%

Toward establishing the presence or absence of horizons in coalescing binaries of compact objects by using their gravitational wave signals

et al. 2022

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The quest for distinguishing black holes from horizonless compact objects using gravitational wave signals from coalescing compact binaries can be helped by utilizing the phenomenon of tidal heating, which leaves its imprint on the binary waveforms through the horizon parameters. These parameters, defined as H 1 and H 2 with H 1;2 ∈ ½0; 1 for the two compact objects, are combined with the binary components' masses and spins to form two new parameters, H eff5 and H eff8 , to minimize their covariances in parameter estimation studies. In this work, we investigate the effects of tidal heating on gravitational waves to probe the observability of these effective parameters. We use a post-Newtonian waveform that includes the phase contribution due to tidal heating as a function of H eff5 and H eff8 , and we examine their 1σ measurement errors as well as the covariances between them mainly using the Fisher matrix approach. Since this approach works well for high signal-to-noise ratios, we focus primarily on the third-generation (3G) gravitational wave detectors Einstein Telescope and Cosmic Explorer and use the second-generation (2G) detector network of LIGO (Hanford, Livingston) and Virgo for comparison. We study how the errors vary with the binaries' total mass, mass ratio, luminosity distance, and component spins. We find that the regions in the total binary mass where measurements of H eff5 and H eff8 are most precise are ∼20-30 M ⊙ for LIGO-Virgo and ∼50-80 M ⊙ for the 3G detectors. Higher component spins allow more precise measurements of H eff5 and H eff8 . For a binary situated at 200 Mpc with component masses 12 M ⊙ and 18 M ⊙ , equal spins χ 1 ¼ χ 2 ¼ 0.8, and H eff5 ¼ 0.6, H eff8 ¼ 12, the 1σ errors in these two parameters are ∼0.01 and ∼0.04, respectively, in 3G detectors. These estimates suggest that precise measurements of the horizon parameters are possible in third-generation detectors, making tidal heating a potential tool to identify the presence or absence of horizons in coalescing compact binaries. We substantiate our results from Fisher studies with a set of Bayesian simulations.

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Gravitational radiation close to a black hole horizon: Waveform regularization and the out-going echo

Cited by 7 publications

References 50 publications

Gravitational wave from extreme mass-ratio inspirals as a probe of extra dimensions

Gravitational wave from extreme mass-ratio inspirals as a probe of extra dimensions

Gravitational-wave echoes from numerical-relativity waveforms via spacetime construction near merging compact objects

Toward establishing the presence or absence of horizons in coalescing binaries of compact objects by using their gravitational wave signals

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