Quasinormal modes of charged fermions in linear dilaton black hole spacetime: exact frequencies

Сакалли, Иззет; Hyusein, Gülnihal Tokgöz

doi:10.3906/fiz-2012-6

Cited by 8 publications

(6 citation statements)

References 61 publications

(62 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Thus, unlike the ordinary or classical normal modes, the amplitude of oscillation decays in time for the QNMs [70]. The QNMs can also be utilized to test the theorem of no-hair, which claims that BHs contain only mass, charge, and angular momentum and for the BH quantization [16,[71][72][73][74][75][76][77][78][79][80][81][82][83][84][85]. Investigating QNMs can therefore provide new insights into physics beyond Einstein's general theory of relativity, which is an important instrumental for the (incomplete) theory of quantum gravity [86].…”

Section: Discussionmentioning

confidence: 99%

“…Investigating QNMs can therefore provide new insights into physics beyond Einstein's general theory of relativity, which is an important instrumental for the (incomplete) theory of quantum gravity [86]. References [87][88][89] provide more detailed reviews of BH QNMs including their various computation methods, which are as follows: 1) Exact solutions [76,84,85,90] 2) WKB approximation [91][92][93][94] 3) Monodromy technique for highly-damped modes [95] 4) Asymptotically AdS BHs: a series solution [96] 5) Asymptotically AdS BHs: the resonance method [97] 6) Continued fraction method [98] 7) Asymptotic iteration method [89,99]…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

Topical Review: Greybody Factors and Quasinormal Modes for Black Holes in Various Theories -- Fingerprints of Invisibles

Sakallı,

Kanzi

2022

Preprint

View full text Add to dashboard Cite

We give a pedagogical introduction to black holes (BHs) greybody factors (GFs) and quasinormal modes (QNMs) and share the recent developments on those subjects. To this end, we present some particular analytical and approximation techniques for the computations of the GFs and QNMs.We first review the gravitational GFs and show how they are analytically calculated for static and spherically symmetric higher dimensional BHs, consisting the charged BHs and existence of cosmological constant (i.e., de Sitter (dS)/anti-de Sitter (AdS)AdS BHs). The computations performed involve both the low-energy (having real and small frequencies) and the asymptotic (having extremely high frequency of the scattered wave throughout the imaginary axis) cases. A generic method is discussed at low frequencies. This method can be used for all three types of spacetime asymptotics and it is unaffected by the BH's features. For asymptotically dS BHs, GF varies depending on whether the spacetime dimension is even or odd, and is proportional to the ratio of the event and cosmic horizon areas. At asymptotic frequencies, the GFs can be computed by using a matching technique inspired by the monodromy method. In the meantime, we also make a general literature review on the matching technique in a separate section. While the GFs for charged or asymptotically dS BHs are generated by non-trivial functions, the GF for asymptotically AdS BHs is precisely one: pure black-body emission. QNMs, which are solutions to the relevant perturbation equations that satisfy the boundary conditions for purely outgoing (gravitational) waves at spatial infinity and purely ingoing (gravitational) waves at the event horizon, are considered using some particular analytical (like the matching technique) and approximation methods. In this study, our primary focus will be on the bosonic and fermionic GFs and QNMs of various BH and brane geometries and reveal the fingerprints of the invisibles with the radiation spectra to be obtained by the WKB approximation and bounding the Bogoliubov coefficients (together with the Miller-Good transformation) methods.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Topical Review: Greybody Factors and Quasinormal Modes for Black Holes in Various Theories -- Fingerprints of Invisibles

Sakallı,

Kanzi

2022

Preprint

View full text Add to dashboard Cite

show abstract

“…To examine NUT's effect on the potentials, we plot the potentials against distance. Figure 1 represents the behavior of the potentials (28) for some specific values of NUT parameter.…”

Section: A Dirac Equationmentioning

confidence: 99%

“…The considered CTNBH solution depends on three parameters: mass M , NUT parameter l, and charge q. We mainly study the spinorial wave dynamics in the geometry of CTNBH with the aid of the Klein-Gordon and Dirac wave equations [19,28]. After having the master equations, we compute the GFs and QNMs of the CTNBH.…”

mentioning

confidence: 99%

Fermionic and Bosonic Greybody Factors as well as Quasinormal Modes for Charged Taub NUT Black Holes

Badawi¹,

Kanzi²,

Сакалли³

2022

Preprint

View full text Add to dashboard Cite

The paper studies the spinorial wave equations, namely the Dirac and the Klein-Gordon equations, as well as the greybody radiations and quasinormal modes (QNMs) of the charged Taub NUT black hole (CTNBH). To obtain fermionic greybody factors (GFs) and QNMs, we study the charged fermions by employing the Dirac equation. To this end, we use a null tetrad in the Newman-Penrose formalism. Then, we separate the Dirac equation into radial and angular sets. Using the obtained radial equations, we convert them into the typical one dimensional Schrödinger-like wave equations with the aid of tortoise coordinate and derive the effective potentials. For bosonic GFs and QNMs, we study the Klein-Gordon equation in the CTNBH geometry and obtain the radial equation. We then derive the effective potential and investigate the effect of NUT parameter on it.We show that while the fermionic QNMs and GFs individually increase with the increasing NUT parameter, the increase of bosonic GFs with increasing NUT parameter is overwhelmingly greater than that of the bosonic QNMs.

show abstract

“…Furthermore, in 2D spacetimes the equations of motion for classical fields simplify and we can study in more detail several physical phenomena, for example, the way in which a 2D black hole reacts when it is perturbed. The QNFs of 2D spacetimes have been studied in recent times (Li et al, 2001;Kettner et al, 2004;Becar et al, 2007;Zelnikov, 2008;López-ortega, 2009;Becar et al, 2010;López-ortega, 2011;López-Ortega and Vega-Acevedo, 2011;Cordero et al, 2012;Myung and Moon, 2012;Estrada-Jiménez et al, 2013;Stetsko, 2017;Jusufi et al, 2018;Sakallı et al, 2018;Mirbabayi, 2020;Bhattacharjee et al, 2021;Kanzi and Sakallı, 2021;Sakalli and Tokgöz Hyusein, 2021). Exact results for the QNFs have previously found (Li et al, 2001;Kettner et al, 2004;Becar et al, 2007;Zelnikov, 2008;López-ortega, 2009;Becar et al, 2010;López-ortega, 2011;López-Ortega and Vega-Acevedo, 2011;Cordero et al, 2012;Myung and Moon, 2012;Estrada-Jiménez et al, 2013;Stetsko, 2017;Jusufi et al, 2018;Sakallı et al, 2018;Mirbabayi, 2020;Bhattacharjee et al, 2021;Kanzi and Sakallı, 2021;Sakalli and Tokgöz Hyusein, 2021), but for some asymptotically adS 2D backgrounds a numerical calculation is necessary (Corder...…”

Section: Introductionmentioning

confidence: 99%

Quasinormal Frequencies of a Two-Dimensional Asymptotically Anti-de Sitter Black Hole of the Dilaton Gravity Theory

Hernández-Velázquez

López-Ortega

2021

Front. Astron. Space Sci.

View full text Add to dashboard Cite

We numerically calculate the quasinormal frequencies of the Klein-Gordon and Dirac fields propagating in a two-dimensional asymptotically anti-de Sitter black hole of the dilaton gravity theory. For the Klein-Gordon field we use the Horowitz-Hubeny method and the asymptotic iteration method for second order differential equations. For the Dirac field we first exploit the Horowitz-Hubeny method. As a second method, instead of using the asymptotic iteration method for second order differential equations, we propose to take as a basis its formulation for coupled systems of first order differential equations. For the two fields we find that the results that produce the two numerical methods are consistent. Furthermore for both fields we obtain that their quasinormal modes are stable and we compare their quasinormal frequencies to analyze whether their spectra are isospectral. Finally we discuss the main results.

show abstract

Quasinormal modes of charged fermions in linear dilaton black hole spacetime: exact frequencies

Abstract: Quasinormal modes of charged fermions in linear dilaton black hole spacetime: Exact frequenciesThe first page should contain the full title in sentence case (e.g., Multiplication modules with Krull dimension)The full names (last names fully capitalised) and affiliations (in English

Cited by 8 publications

References 61 publications

Topical Review: Greybody Factors and Quasinormal Modes for Black Holes in Various Theories -- Fingerprints of Invisibles

Topical Review: Greybody Factors and Quasinormal Modes for Black Holes in Various Theories -- Fingerprints of Invisibles

Fermionic and Bosonic Greybody Factors as well as Quasinormal Modes for Charged Taub NUT Black Holes

Quasinormal Frequencies of a Two-Dimensional Asymptotically Anti-de Sitter Black Hole of the Dilaton Gravity Theory

Contact Info

Product

Resources

About