No stable wormholes in Einstein-dilaton-Gauss-Bonnet theory

Cuyubamba, M. A.; Konoplya, R. A.; Zhidenko, A.

doi:10.1103/physrevd.98.044040

Cited by 52 publications

(45 citation statements)

References 87 publications

(124 reference statements)

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“…Quasinormal modes of wormholes have been recently studied in a number of papers in the context of possi- ble astrophysical observations, testing wormhole geometry and stability [38][39][40][41][42][43][44][45][46][47]. Here we were interested in the question whether the arbitrarily long-lived quasinormal modes, which exist in the spectra of massive fields in some black-hole backgrounds, are also present in the spectra of wormholes?…”

Section: Discussionmentioning

confidence: 99%

Arbitrarily long-lived quasinormal modes in a wormhole background

2020

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Arbitrarily long lived modes, called quasi-resonances, are known to exist in the spectrum of massive fields for a number of black-hole backgrounds at some discrete values of mass of the field. Here we show that these modes also exist in the background of wormholes, unless a wormhole has a constant red-shift function, that is, tideless in the radial direction. The evidence of quasi-resonances is supported by calculations in the frequency and time domains, which are in a good concordance. At large masses of the field, time-domain profiles of the absolute value of the wave function have peculiar behavior: the long-lived modes dominate in the signal after a long period of power-law tails.

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Section: Discussionmentioning

confidence: 99%

Arbitrarily long-lived quasinormal modes in a wormhole background

2020

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“…BHs under specific boundary conditions, corresponding to purely outgoing waves at infinity and purely incoming waves at the event horizon (minus infinity in terms of the tortoise coordinate). The boundary conditions for a traversable wormhole which connects two infinities are the same in terms of the tortoise coordinate [45], so that many of the tools used for finding BH quasinormal modescan, with small modifications, be used for wormholes as well [37,46,47,59,60,62,63]. In particular, to finding the frequencies of quasinormal modes, we will use the WKB method when the effective potential has a single maximum and time domain integration for all types of the effective potentials.…”

Section: Quasinormal Modes Of Bhs Are Proper Oscillations Ofmentioning

confidence: 99%

Echoes in brane worlds: Ringing at a black hole-wormhole transition

Бронников

Konoplya

2020

Phys. Rev. D

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Echoes are known as modifications of the usual quasinormal ringing of a black hole at late times because of the deviation of space-time from the initial black-hole geometry in a small region near its event horizon. We consider a class of brane-world model solutions of the Shiromizu-Maeda-Sasaki equations, which describe both black holes and wormholes and interpolate between them via a continuous parameter. In this way the brane-world scenario provides a natural model for wormholes mimicking the black hole behavior if the continuous parameter is chosen near the threshold with a black-hole solution. We show that in the vicinity of this threshold interpolating between black holes and wormholes, quasinormal ringing of the wormholes at the initial stage is indistinguishable from that of the black holes with nearby values of the above parameter, but at later times the signal is modified by intensive echoes. We notice that the black-hole mimickers that are wormholes near the threshold have the largest quality factor and are therefore the best oscillators among the considered examples.

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“…Quasinormal modes of the wormholes, connecting two infinities, obey the same boundary conditions in terms of the tortoise coordinate as those for black holes and they were studied in various contexts in [15][16][17][18][19][20][21][22][23][24][25][26][27] An interesting model interpolating between the traversable wormhole and regular black hole was suggested in [1] and extended to the time-dependent case in [2]. Here we would like to see how the transition between the regular black hole and a wormhole via black bounce can look like from the point of view of quasinormal ringing.…”

Section: Introductionmentioning

confidence: 99%

Ringing of the regular black-hole/wormhole transition

Churilova¹,

Stuchlík²

2020

Class. Quantum Grav.

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Recently a simple one-parameter generalization of the Schwarzschild spacetime was suggested by A. M. Visser [JCAP 1902, 042 (2019)] as a toy model describing the regular black hole and traversable wormhole states separated by the border (one-way wormhole) state, depending on the value of the new parameter. Here we will study quasinormal modes of all three states and show that the black-hole/wormhole transition is characterized by echoes, while the memory of the black hole state is kept in the time-domain profile of the wormhole perturbation at the initial stage of the exponential fall off. Calculations of quasinormal modes with the help of the WKB method with Padé expansion and time-domain integration are in a good agreement. An analytical formula for quasinormal modes in the eikonal regime is obtained.

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No stable wormholes in Einstein-dilaton-Gauss-Bonnet theory

Cited by 52 publications

References 87 publications

Arbitrarily long-lived quasinormal modes in a wormhole background

Arbitrarily long-lived quasinormal modes in a wormhole background

Echoes in brane worlds: Ringing at a black hole-wormhole transition

Ringing of the regular black-hole/wormhole transition

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