2012

DOI: 10.1103/physrevd.86.124008

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Quasinormal modes for the scattering on a naked Reissner-Nordström singularity

Cecilia Chirenti

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Abstract: What should be the quasinormal modes associated with a spacetime that contains a naked singularity instead of a black hole? In the present work we address this problem by studying the scattering of scalar fields on a curved background described by a Reissner-Nordström spacetime with |q| > m. We show that there is a qualitative difference between cases with 1 < q 2 /m 2 9/8 and cases with q 2 /m 2 9/8. We discuss the necessary conditions for the well-posedness of the problem, and present results for the low dam… Show more

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Cited by 20 publications

(25 citation statements)

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“…The problem is also apparent by seeing that the allowed solutions in this case can imply a loss of unitarity (a net flux in or out of the singularity). To obtain a sensible boundary condition for the RNN spacetime one might impose unitarity as an external constraint [35]. This is not necessary for the other spacetimes.…”

Section: Regular Field Dynamicsmentioning

confidence: 99%

Not quite a black hole

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2017

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Astrophysical black hole candidates, although long thought to have a horizon, could be horizonless ultra-compact objects. This intriguing possibility is motivated by the black hole information paradox and a plausible fundamental connection with quantum gravity. Asymptotically free quadratic gravity is considered here as the UV completion of general relativity. A classical theory that captures its main features is used to search for solutions as sourced by matter. We find that sufficiently dense matter produces a novel horizonless configuration, the 2-2-hole, which closely matches the exterior Schwarzschild solution down to about a Planck proper length of the would-be horizon. The 2-2-hole is characterized by an interior with a shrinking volume and a seemingly innocuous timelike curvature singularity. The interior also has a novel scaling behavior with respect to the physical mass of the 2-2-hole. This leads to an extremely deep gravitational potential in which particles get efficiently trapped via collisions. As a generic static solution, the 2-2-hole may then be the nearly black endpoint of gravitational collapse. There is a considerable time delay for external probes of the 2-2-hole interior, and this determines the spacing of echoes in a post-merger gravitational wave signal.Comment: 35 pages, 11 figures, added section IIID: A brick wall and entrop

“…The problem is also apparent by seeing that the allowed solutions in this case can imply a loss of unitarity (a net flux in or out of the singularity). To obtain a sensible boundary condition for the RNN spacetime one might impose unitarity as an external constraint [35]. This is not necessary for the other spacetimes.…”

Section: Regular Field Dynamicsmentioning

confidence: 99%

Not quite a black hole

¹

,

²

2017

View full text Add to dashboard Cite

Astrophysical black hole candidates, although long thought to have a horizon, could be horizonless ultra-compact objects. This intriguing possibility is motivated by the black hole information paradox and a plausible fundamental connection with quantum gravity. Asymptotically free quadratic gravity is considered here as the UV completion of general relativity. A classical theory that captures its main features is used to search for solutions as sourced by matter. We find that sufficiently dense matter produces a novel horizonless configuration, the 2-2-hole, which closely matches the exterior Schwarzschild solution down to about a Planck proper length of the would-be horizon. The 2-2-hole is characterized by an interior with a shrinking volume and a seemingly innocuous timelike curvature singularity. The interior also has a novel scaling behavior with respect to the physical mass of the 2-2-hole. This leads to an extremely deep gravitational potential in which particles get efficiently trapped via collisions. As a generic static solution, the 2-2-hole may then be the nearly black endpoint of gravitational collapse. There is a considerable time delay for external probes of the 2-2-hole interior, and this determines the spacing of echoes in a post-merger gravitational wave signal.Comment: 35 pages, 11 figures, added section IIID: A brick wall and entrop

“…It was found a critical q value for shadow existence, namely for q ≤ 9/8, Reissner -Nordström black holes have shadows while for q > 9/8 the shadows do not exist. Interestingly, the same critical value is responsible for a qualitative different behavior of quasinormal modes for the scattering [30] and for existence of circular orbits of neutral test particles [31].…”

Section: Introductionmentioning

confidence: 96%

Constraints on a charge in the Reissner-Nordström metric for the black hole at the Galactic Center

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2014

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Using an algebraic condition of vanishing discriminant for multiple roots of fourth degree polynomials we derive an analytical expression of a shadow size as a function of a charge in the Reissner -Nordström (RN) metric [1,2]. We consider shadows for negative tidal charges and charges corresponding to naked singularities q = Q 2 /M 2 > 1, where Q and M are black hole charge and mass, respectively, with the derived expression. An introduction of a negative tidal charge q can describe black hole solutions in theories with extra dimensions, so following the approach we consider an opportunity to extend RN metric to negative Q 2 , while for the standard RN metric Q 2 is always non-negative. We found that for q > 9/8 black hole shadows disappear. Significant tidal charges q = −6.4 (suggested by Bin-Nun [3-5]) are not consistent with observations of a minimal spot size at the Galactic Center observed in mm-band, moreover, these observations demonstrate that a Reissner -Nordström black hole with a significant charge q ≈ 1 provides a better fit of recent observational data for the black hole at the Galactic Center in comparison with the Schwarzschild black hole.

“…

This is a review of my work published in the papers [1][2][3][4]. It offers a more detailed discussion of the results than what was given in the published papers and it links my results to some conclusions recently made by other people.

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confidence: 79%

Quantization of Horizon Entropy and the Thermodynamics of Spacetime

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2014

Self Cite

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This is a review of my work published in the papers [1][2][3][4]. It offers a more detailed discussion of the results than what was given in the published papers and it links my results to some conclusions recently made by other people. It also offers some new arguments for the conclusions previously made. The fundamental idea of this work is that the semi-classical quantization of the black hole entropy, as suggested by Bekenstein [5], holds (at least) generically for the spacetime horizons. We support this conclusion by two separate arguments: 1. we generalize Bekenstein's lower bound on the horizon area transition to much larger class of horizons than only the black hole horizon, 2. we obtain the same entropy spectra via the asymptotic quasi-normal frequencies of some particular spherically symmetric multi-horizon spacetimes, (in the way proposed by Maggiore [6]). The main result of this paper supports the conclusions made by other people in [7,8], but uses different arguments.

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