Can the abyss swallow gravitational waves or why do we not observe echoes?

Zhidenko, A.

doi:10.1209/0295-5075/ac6e00

Cited by 7 publications

(2 citation statements)

References 33 publications

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“…Here, we shall study the quasinormal modes from the wormholes for the scalar (field) perturbations and Dirac (field) perturbations using WKB approximation method. We shall neglect any possible echoes from quantum corrections near the wormhole throat or from any matter far from it [119,141].…”

Section: Quasinormal Modesmentioning

confidence: 99%

Tideless traversable wormholes surrounded by cloud of strings in f(R) gravity

Gogoi

Goswami

2023

J. Cosmol. Astropart. Phys.

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We study the tideless traversable wormholes in the f(R) gravity metric formalism. First we consider three shape functions of wormholes and study their viabilities and structures. The connection between the f(R) gravity model and wormhole shape function has been studied and the dependency of the f(R) gravity model with the shape function is shown. We also obtain a wormhole solution in the f(R) gravity Starobinsky model surrounded by a cloud of strings. In this case, the wormhole shape function depends on both the Starobinsky model parameter and the cloud of strings parameter. The structure and height of the wormhole is highly affected by the cloud of strings parameter, while it is less sensitive to the Starobinsky model parameter. The energy conditions have been studied and we found the ranges of the null energy condition violation for all wormhole structures. The quasinormal modes from these wormhole structures for the scalar and Dirac perturbations are studied using higher order WKB approximation methods. The quasinormal modes for the toy shape functions depend highly on the model parameters. In case of the Starobinsky model's wormhole the quasinormal frequencies and the damping rate increase with an increase in the Starobinsky model parameter in scalar perturbation. Whereas in Dirac perturbation, with an increase in the Starobinsky model parameter the quasinormal frequencies decrease and the damping rate increases. The cloud of strings parameter also impacts prominently and differently the quasinormal modes from the wormhole in the Starobinsky model.

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Section: Quasinormal Modesmentioning

confidence: 99%

Tideless traversable wormholes surrounded by cloud of strings in f(R) gravity

Gogoi

Goswami

2023

J. Cosmol. Astropart. Phys.

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“…In particular, Cardoso suggests using gravitational wave echoes as a brand-new characteristic of unusual compact objects [47]. Gravitational wave echoes were later found in the late stage of quasinormal ringing when QNM was explored in various space-time contexts [48][49][50][51][52][53][54][55][56][57][58][59]. They are eager to use it to distinguish between various compact objects.…”

Section: Jcap05(2024)019mentioning

confidence: 99%

The quantum corrected Schwarzschild black hole with a linear-quadratic GUP: a comprehensive evaluation

Barman,

Al-Badawi,

Jha

et al. 2024

J. Cosmol. Astropart. Phys.

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In this manuscript, we delve into an analytic and numerical probe of shadow with different accretion models, quasinormal modes, Hawking radiation, and gravitational lensing to study observational impacts of quantum effect introduced through linear-quadratic GUP(LQG). Our investigation reveals that the shadows of LQG-modified black holes are smaller and brighter than Schwarzschild black holes. To examine the impact of the quantum correction on the quasinormal mode, linear-quadratic GUP-modified black holes are explored under scalar and electromagnetic field perturbation. Here, linear-quadratic GUP is used to capture quantum corrections. It is observed that the incorporation of quantum correction by linear-quadratic GUP alters the singularity structure of the black hole. To compute the quasinormal modes of this linear-quadratic GUP-inspired quantum-corrected black holes, we compute the effective potential generated under the perturbation of scalar and electromagnetic field, and then we use the sixth-order WKB approach in conjunction with the appropriate numerical analysis. We find that the greybody factor decreases with the GUP parameter α implying that the probability of transmission decreases with the GUP parameter. The total power emitted by LQG modified black hole is found to be greater than that emitted by Schwarzschild black hole. Finally, we study weak gravitational lensing and make a comparison with quadratic GUP and linear GUP-modified black holes.

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