Imprint of black hole area quantization and Hawking radiation on inspiraling binary

Datta, Sayak; Phukon, K. S.

doi:10.1103/physrevd.104.124062

Cited by 17 publications

(4 citation statements)

References 67 publications

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“…Therefore, we can conclude that the Hawking radiation power emitted is also quantized and the quantization is affected by the Lorentz violation. Recent studies show the impacts of area quantization of black holes on GW echoes [44][45][46]. So, it can be possible in the near future to comment on the fate of quantum gravity and Lorentz violation provided we have sufficient astrophysical signatures.…”

Section: Jcap06(2022)029mentioning

confidence: 99%

“…Finally, we perform a study on the area of the black holes with the help of the adiabatic invariance method. Since, the area of black holes is connected with the GW echo [44][45][46], entropy spectrum and power spectrum of black holes, we believe the results can be further used to study the impacts of Lorentz violation on different aspects of black holes.…”

Section: Introductionmentioning

confidence: 97%

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Quasinormal modes and Hawking radiation sparsity of GUP corrected black holes in bumblebee gravity with topological defects

Gogoi

Goswami

2022

J. Cosmol. Astropart. Phys.

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We have obtained the Generalized Uncertainty Principle (GUP) corrected de Sitter and anti-de Sitter black hole solutions in bumblebee gravity with a topological defect. We have calculated the scalar, electromagnetic and gravitational quasinormal modes for the both vanishing and non-vanishing effective cosmological constant using Padé averaged sixth order WKB approximation method. Apart from this, the time evolutions for all three perturbations are studied, and quasinormal modes are calculated using the time domain profile. We found that the first order and second order GUP parameters α and β, respectively have opposite impacts on the quasinormal modes. The study also finds that the presence of a global monopole can decrease the quasinormal frequencies and the decay rate significantly. On the other hand, Lorentz symmetry violation has noticeable impacts on the quasinormal frequencies and the decay rate. We have studied the greybody factors, power spectrum and sparsity of the black hole with the vanishing effective cosmological constant for all the three perturbations. The presence of Lorentz symmetry breaking and the GUP parameter α decrease, while other GUP parameter β and the presence of global monopole increase the probability of Hawking radiation to reach the spatial infinity. The presence of Lorentz violation can make the black holes less sparse, while the presence of a global monopole can increase the sparsity of the black holes. Moreover, we have seen that the black hole area quantization rule is modified by the presence of Lorentz symmetry breaking.

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Section: Jcap06(2022)029mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 97%

Quasinormal modes and Hawking radiation sparsity of GUP corrected black holes in bumblebee gravity with topological defects

Gogoi

Goswami

2022

J. Cosmol. Astropart. Phys.

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“…This remarkable feature of area quantization has observational consequences which include differences between the usual Hawking behavior from that of LQG [14], a distorted ringdown signal, or the presence of latetime echoes. Indeed, the ringdown signal from the merger of a binary black hole, as computed from general relativity, is described very well by the quasinormal modes of the final Kerr black hole (see, for example, [15][16][17]).…”

Section: A Minimal Modelmentioning

confidence: 99%

Minimal model for the Bekenstein-Hawking entropy

Bargueño

Contreras

2022

Phys. Rev. D

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In this work we derive the Bekenstein-Hawking entropy formula, S ¼ A 4l 2 p , from the following minimal assumptions: (i) there is a minimum area, A min , proportional to l 2 p ; (ii) the event horizon area, A, is tessellated by N ¼ A=A min distinguishable units; and (iii) the internal structure of these units is that of an infinite tower of internal levels. Although our results are model independent, this internal structure can be realized as the excitations of more fundamental entities such as, for instance, strings or loop quantum gravity spin networks. Even more, once the microstates of the black hole are taken to be singlets formed within the infinite tower of states describing the whole event horizon, the correction term − 3 2 log A emerges from our model. Finally, some comments regarding the applicability of the present model to extremal black holes, as well as possible relationships with spectral geometry and other approaches are pointed out. Our results are independent of the dimension of the black hole and whether it is rotating or not.

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“…The effect of TH on objects such as NSs or horizonless ECOs is comparatively much less due to their lack of a horizon. So, a careful measurement of this phase shift can be used in principle to distinguish BHs from horizonless compact objects [36,39,[55][56][57][58][59][60][61][62][63].…”

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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Imprint of black hole area quantization and Hawking radiation on inspiraling binary

Cited by 17 publications

References 67 publications

Quasinormal modes and Hawking radiation sparsity of GUP corrected black holes in bumblebee gravity with topological defects

Quasinormal modes and Hawking radiation sparsity of GUP corrected black holes in bumblebee gravity with topological defects

Minimal model for the Bekenstein-Hawking entropy

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

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