Inverse spectrum problem for quasi-stationary states

Völkel, Sebastian H.

doi:10.1088/2399-6528/aaaee2

Cited by 12 publications

(8 citation statements)

References 25 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…If the spectrum is not known analytically, but as a discrete set of complex numbers, one has to interpolate between the states in order to obtain a discrete function for T (E). From here one can already expect that the accuracy of the reconstruction improves for potentials with a large number of trapped modes compared to ones with a smaller number, see [3,34] for discussions. With the reconstruction of (L 1 , L 2 ) one has two equations for four turning points (x 0 , x 1 , x 2 , x 3 ).…”

Section: A Outline Of the Methodsmentioning

confidence: 74%

See 1 more Smart Citation

Wormhole potentials and throats from quasi-normal modes

Völkel

Kokkotas

2018

Class. Quantum Grav.

Self Cite

View full text Add to dashboard Cite

Exotic compact objects refer to a wide class of black hole alternatives or effective models to describe phenomenologically quantum gravitational effects on the horizon scale. In this work we show how the knowledge of the quasi-normal mode spectrum of non-rotating wormhole models can be used to reconstruct the effective potential that appears in the perturbation equations. From this it is further possible to obtain the parameters that characterize the specific wormhole model, which in this paper was chosen to be the one by Damour and Solodukhin. We also address the question whether one can distinguish such type of wormholes from ultra compact stars, if only the quasi-normal mode spectrum is known. We have proven that this is not possible by using the trapped modes only, but requires additional information.The here presented inverse method is an extension of work that has previously been developed and applied to the oscillation spectra of ultra compact stars and gravastars. However, it is not limited to the study of exotic compact objects, but applicable to symmetric double barrier potentials that appear in one-dimensional wave equations. Therefore we think it can be of interest for other fields too. * sebastian.voelkel@uni-tuebingen.de arXiv:1802.08525v2 [gr-qc]

show abstract

Section: A Outline Of the Methodsmentioning

confidence: 74%

“…In cases where the widths are reconstructed without any pathologies 8 , it can still happen that the reconstructed potential is unphysical due to "overhanging cliffs", which can come from the very large values of L 2 (E) for small values of E around E min . For an extended discussion of this effect we refer to [3,34].…”

Section: A Accuracymentioning

confidence: 99%

Wormhole potentials and throats from quasi-normal modes

Völkel

Kokkotas

2018

Class. Quantum Grav.

Self Cite

View full text Add to dashboard Cite

show abstract

“…The reverse-engineering of the process, i.e., a reconstruction of the scattering potential V from a mode measurement was proposed in Ref. [113,307,308]. The impact of measurement error on such reconstruction is yet to be assessed.…”

Section: Quasinormal Modesmentioning

confidence: 99%

Testing the nature of dark compact objects: a status report

2019

View full text Add to dashboard Cite

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.

show abstract

“…Let us now consider scenario where the QNM spectrum is known empirically, and discuss to what extent this information can be used to constrain the coefficients appearing in our effective action. This procedure goes under the name of "inverse problem"-see for example [62,63]. In our analysis, we will resort to a WKB approximation, and restrict ourselves to the case where the background metric is a "small" deviation from Schwarzschild.…”

Section: From the Qnm Spectrum To The Effective Potential: The Inversmentioning

confidence: 99%

Effective field theory of black hole quasinormal modes in scalar-tensor theories

Franciolini¹,

Hui

Penco

et al. 2019

J. High Energ. Phys.

149

View full text Add to dashboard Cite

The final ringdown phase in a coalescence process is a valuable laboratory to test General Relativity and potentially constrain additional degrees of freedom in the gravitational sector. We introduce here an effective description for perturbations around spherically symmetric spacetimes in the context of scalar-tensor theories, which we apply to study quasinormal modes for black holes with scalar hair. We derive the equations of motion governing the dynamics of both the polar and the axial modes in terms of the coefficients of the effective theory. Assuming the deviation of the background from Schwarzschild is small, we use the WKB method to introduce the notion of "light ring expansion". This approximation is analogous to the slow-roll expansion used for inflation, and it allows us to express the quasinormal mode spectrum in terms of a small number of parameters. This work is a first step in describing, in a model independent way, how the scalar hair can affect the ringdown stage and leave signatures on the emitted gravitational wave signal. Potential signatures include the shifting of the quasi-normal spectrum, the breaking of isospectrality between polar and axial modes, and the existence of scalar radiation. arXiv:1810.07706v3 [hep-th] 1 Feb 2019 F The Regge-Wheeler equations 44 G Isolating the gravitational waves -the large radius limit 44 H Bianchi identities 46 -1 -out. The non-invariance under shifts of the Hamiltonian constraints, responsible for this fact, is at the core of the construction of shift-symmetric adiabatic modes on FLRW spacetimes [33, 34]. 6In other words, the relevant potential for the odd modes depends exclusively on the background metric components, with exactly the same functional dependence as in GR. This still leaves open the possibility of a modification to the odd QNM spectrum if the metric is different from Schwarzschild.

show abstract

Inverse spectrum problem for quasi-stationary states

Cited by 12 publications

References 25 publications

Wormhole potentials and throats from quasi-normal modes

Wormhole potentials and throats from quasi-normal modes

Testing the nature of dark compact objects: a status report

Effective field theory of black hole quasinormal modes in scalar-tensor theories

Contact Info

Product

Resources

About