Tidal heating of black holes and exotic compact objects on the brane

Chakraborty, Sumanta; Datta, Sayak; Sau, Subhadip

doi:10.48550/arxiv.2103.12430

Cited by 12 publications

(14 citation statements)

References 54 publications

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“…In previous studies, a stability analysis led also to observable effects such as echoes of braneworld compact objects [55,56], as well as other exotic compact objects [95][96][97]. A natural question emerges of whether gravitational waves from black hole mergers or other astrophysical processes could provide evidence for extra dimensions and distinguish brane-world solutions of this type from the corresponding four-dimensional ones [57]. Could we construct alternative localised black-hole solutions by considering different forms of the metric function f (ρ), such as the Schwarzschild-Rindler-(Anti-)de Sitter solution with an additional linear term associated with dark matter or scalar-hair effects [98], and what would be in that case the profile of the bulk matter?…”

Section: Epiloguementioning

confidence: 98%

Analytic and exponentially localized brane-world Reissner-Nordström-AdS solution: a top-down approach

Nakas,

Kanti

2021

Preprint

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In this work, we construct a five-dimensional spherically-symmetric, charged and asymptotically Anti-de Sitter black hole with its singularity being point-like and strictly localised on our brane. In addition, the induced brane geometry is described by a Reissner-Nordström-(A)dS line-element. We perform a careful classification of the horizons, and demonstrate that all of them are exponentially localised close to the brane thus exhibiting a pancake shape. The bulk gravitational background is everywhere regular, and reduces to an AdS 5 spacetime right outside the black-hole event horizon. This geometry is supported by an anisotropic fluid with only two independent components, the energy density ρ E and tangential pressure p 2 . All energy conditions are respected close to and on our brane, but a local violation takes place within the event horizon regime in the bulk. A tensor-vector-scalar field-theory model is built in an attempt to realise the necessary bulk matter, however, in order to do so, both gauge and scalar degrees of freedom need to turn phantom-like at the bulk boundary. The study of the junction conditions reveals that no additional matter needs to be introduced on the brane for its consistent embedding in the bulk geometry apart from its constant, positive tension. We finally compute the effective gravitational equations on the brane, and demonstrate that the Reissner-Nordström-(A)dS geometry on our brane is caused by the combined effect of the five-dimensional geometry and bulk matter with its charge being in fact a tidal charge.

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Section: Epiloguementioning

confidence: 98%

Analytic and exponentially localized brane-world Reissner-Nordström-AdS solution: a top-down approach

Nakas,

Kanti

2021

Preprint

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“…We will only need to use a window function when evaluating the integral(-part) of ( 35) to remove any contribution from r > r max in Tlmω [Eq. (32)] . We specifically used a window of (1 − tanh(2(r − r max ))/M)/2.…”

Section: B Effective One Body (Eob) Quasi-circular Plungementioning

confidence: 99%

“…A complementary way way to model gravitational waves from ECOs, by parametrizing the compactness of objects, is proposed in [27]. During the inspiral stage, the absence of horizon in ECOs also modifies the tidal interaction within the binary, and leads to additional signatures in gravitational waves [28][29][30][31][32].…”

Section: Introductionmentioning

confidence: 99%

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

Srivastava,

Chen

2021

Preprint

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Black hole perturbation theory for Kerr black holes is best studied in the Newman Penrose (NP) Formalism, in which gravitational waves are described as perturbations in the Weyl scalars ψ 0 and ψ 4 , with the governing equation being the well-known Teukolsky equation. Near infinity and near the horizon, ψ 4 is dominated by the component that corresponds to waves propagating towards the positive radial direction, while ψ 0 is dominated by the component that corresponds to waves that propagate towards the negative radial direction. Since gravitational-wave detectors measure out-going waves at infinity, research has been mainly focused on ψ 4 , leaving ψ 0 less studied. But the scenario is reversed in the near horizon region where the in-going-wave boundary condition needs to be imposed. Thus, the near horizon phenomena, e.g., tidal heating and gravitational-wave echoes from Extremely Compact Objects (ECOs), requires computing ψ 0 . In this work, we explicitly calculate the source term for the ψ 0 Teukolsky equation due to a point particle plunging into a Kerr black hole. We highlight the need to regularize the solution of the ψ 0 Teukolsky equation obtained using the usual Green's function techniques. We suggest a regularization scheme for this purpose and go on to compute the ψ 0 waveform close to a Schwarzschild horizon for two types of trajectories of the in-falling particle. We compare the ψ 0 waveform calculated directly from the Teukolsky equation with the ψ 0 waveform obtained by using the Starobinsky-Teukolsky identity on ψ 4 . We also compute the first out-going gravitational-wave echo waveform near infinity, using the near-horizon ψ 0 computed directly from the Teukolsky equation, and the Boltzmann boundary condition on the ECO surface. We show that this out-going echo is quantitatively very different (stronger) than the echo obtained using previous prescriptions that did not compute the near-horizon ψ 0 directly using the Teukolsky equation.

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“…One of the very intriguing questions in fundamental physics is how gravity behaves in the quantum regime. Since GWs bring information from the very close vicinity of BHs, it is expected that GWs may shed some light on this mystery [35][36][37][38][39][40][41]. The idea behind such expectations follows from the fact that the Planck scale physics may affect the tidal Love numbers of the compact objects [11,12].…”

Section: Introduction-mentioning

confidence: 99%