Can We Probe Planckian Corrections at the Horizon Scale with Gravitational Waves?

Addazi, Andrea; Marcianò, Antonino; Yunes, Nicolás

doi:10.1103/physrevlett.122.081301

Cited by 46 publications

(64 citation statements)

References 71 publications

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“…15). Due to the logarithmic scaling, in these models the statistical errors on would depend exponentially on the TLNs and reaching a Planckian requires a very accurate measurement of k [407]. Nonetheless, this does not prevent to perform ECO model selection (see Fig.…”

Section: Tidal Deformabilitymentioning

confidence: 99%

Testing the nature of dark compact objects: a status report

2019

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Very compact objects probe extreme gravitational fields and may be the key to understand outstanding puzzles in fundamental physics. These include the nature of dark matter, the fate of spacetime singularities, or the loss of unitarity in Hawking evaporation. The standard astrophysical description of collapsing objects tells us that massive, dark and compact objects are black holes. Any observation suggesting otherwise would be an indication of beyond-the-standard-model physics. Null results strengthen and quantify the Kerr black hole paradigm. The advent of gravitationalwave astronomy and precise measurements with very long baseline interferometry allow one to finally probe into such foundational issues. We overview the physics of exotic dark compact objects and their observational status, including the observational evidence for black holes with current and future experiments.

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Section: Tidal Deformabilitymentioning

confidence: 99%

Testing the nature of dark compact objects: a status report

2019

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“…We would like to thank Bruce Allen, Vitor cardoso, Badri Krishnan, Alex working support by the COST Action GWverse CA16104. 5 The uncertainty principle of quantum gravity may set a fundamental resolution limit to GW observations that is well above the Planckian scale [70]. Our estimate is different from [70] as we do not measure any Planckian effect and the lower bound on the entropy partially comes from a theoretical consideration.…”

Section: Acknowledgmentsmentioning

confidence: 74%

Lower limit on the entropy of black holes as inferred from gravitational wave observations

2019

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Black hole (BH) thermodynamics was established by Bekenstein and Hawking, who made abstract theoretical arguments about the second law of thermodynamics and quantum theory in curved spacetime respectively. Testing these ideas experimentally has, so far, been impractical because the putative flux of Hawking radiation from astrophysical BHs is too small to be distinguished from the rest of the hot environment. Here, it is proposed that the spectrum of emitted gravitational waves (GWs) after the merger of two BHs, in particular the spectrum of GW150914, can be used to infer a lower limit on the magnitude of the entropy of the post-merger BH. This lower bound is potentially significant as it could be of the same order as the Bekenstein-Hawking entropy. To infer this limit, we first assume that the result of the merger is an ultracompact object with an external geometry which is Schwarzschild or Kerr, but with an outer surface which is capable of reflecting in-falling GWs rather than fully absorbing them. If the absence of deviations from the predictions of general relativity in detected GW signals will be verified, we will then obtain a bound on the minimal redshift factor of GWs that emerge from the vicinity of the object's surface. This lack of deviations would also mean that the remnant of the merger has to have a strongly absorbing surface and must then be a BH for all practical purposes. We conclude that a relationship between the minimal redshift factor and the BH entropy, which was first proposed by 't Hooft, could then be used to set a lower bound on the entropy of the post-merger BH.

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“…In a binary system the TD phase takes into account the response of one of the two objects to the external gravitational field of the other, and the effect can be parametrized in terms of the so-called Love numbers, which can be non-zero for a horizonless object [89][90][91][92]. The non-zero leading term for the phase TD in the PN expansion is given by [83,93] TD ( f ) = − N 6M 5 v 10 (1 + q) 2 q ,…”

Section: Love Numbersmentioning

confidence: 99%

Phenomenology of GUP stars

et al. 2020

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We study quantum corrections at the horizon scale of a black hole induced by a Generalized Uncertainty Principle (GUP) with a quadratic term in the momentum. The interplay between quantum mechanics and gravity manifests itself into a non-zero uncertainty in the location of the black hole radius, which turns out to be larger than the usual Schwarzschild radius. We interpret such an effect as a correction which makes the horizon disappear, as it happens in other models of quantum black holes already considered in literature. We name this kind of horizonless compact objects GUP stars. We also investigate some phenomenological aspects in the astrophysical context of binary systems and gravitational wave emission by discussing Love numbers, quasi-normal modes and echoes, and studying their behavior as functions of the GUP deformation parameter. Finally, we preliminarily explore the possibility to constrain such a parameter with future astrophysical experiments.

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Can We Probe Planckian Corrections at the Horizon Scale with Gravitational Waves?

Cited by 46 publications

References 71 publications

Testing the nature of dark compact objects: a status report

Testing the nature of dark compact objects: a status report

Lower limit on the entropy of black holes as inferred from gravitational wave observations

Phenomenology of GUP stars

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