Quasinormal modes and absorption probabilities of spin-
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 fields in 
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-dimensional Reissner-Nordström black hole spacetimes

Chen, C.-H.; Cho, H. T.; Cornell, Alan S.; Harmsen, Gerhard; Ngcobo, X.

doi:10.1103/physrevd.97.024038

Cited by 11 publications

(27 citation statements)

References 16 publications

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“…For the Rarita-Schwinger case, L = L + 1/2 = κ = ℓ + 2 = j + 1/2 for ℓ ∈ N o and j = 3/2, 5/2, ... [55][56][57][58].…”

Section: A the Dolan-ottewill Expansion Methodsmentioning

confidence: 99%

“…For maximally-symmetric BH spacetimes, the effective Dirac [35,[51][52][53][54] and Rarita-Schwinger [55][56][57][58] potentials have a supersymmetric form,…”

Section: B Half-integer Spin Perturbationsmentioning

confidence: 99%

“…As shall be shown, the potentials are further categorised within the spin-3/2 framework into transverse traceless (TT) and non-transverse traceless (non-TT) eigenmodes in order to describe the perturbations of d-dimensional, spherically-symmetric BHs fully, according to the gauge-invariant formalism constructed in Refs. [55][56][57][58]. Since TT modes emerge only for d ≥ 5, their study is confined to this analytical section.…”

Section: B Half-integer Spin Perturbationsmentioning

confidence: 99%

“…We may now turn to Ref. [57], where a study of the spin-3/2 perturbations of higherdimensional RN BHs yielded TT eigenmodes for which the potentials V 1,2 were defined in terms of…”

Section: Spin-3/2 Perturbationsmentioning

confidence: 99%

“…Less common are studies on the spin-3/2 QNFs. From the gauge-invariant formalism constructed by some of the authors, results have been obtained for spin-3/2 QNFs via Konoplya's 6th-order WKB and improved AIM in Schwarzschild-Tangherlini contexts [56], via the CFM for the RN BH spacetime [57], and via the Horowitz-Hubeny approach for S(A)dS cases with d ≥ 5 [58]. A major component of this section is thus to add to the extant results for the QNFs of half-integer fields by applying Dolan and Ottewill's inverse multipolar expansion method [38] to the spin-3/2 fields, as well as spin-1/2 fields in the RN context, for the first time.…”

Section: While Numerical Techniques Have Been Exploited Extensively I...mentioning

confidence: 99%

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Quasinormal modes for integer and half-integer spins within the large angular momentum limit

Chen,

Cho,

Chrysostomou

et al. 2021

Preprint

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While independent observations have been made regarding the behaviour of effective quasinormal mode (QNM) potentials within the large angular momentum limit, we demonstrate analytically here that a uniform expression emerges for non-rotating, higher-dimensional, and sphericallysymmetric black holes (BHs) in this regime for fields of integer and half-integer spin in asymptotically flat and dS BH contexts; a second uniform expression arises for these QNM potentials in AdS BH spacetimes. We then proceed with a numerical analysis based on the multipolar expansion method recently proposed by Dolan and Ottewill to determine the behaviour of quasinormal frequencies (QNF) for varying BH parameters in the eikonal limit. We perform a complete study of Dolan and Ottewill's method for perturbations of spin s ∈ {0, 1/2, 1, 3/2, 2} in 4D Schwarzschild, Reissner-Nordström, and Schwarzschild de Sitter spacetimes, clarifying expressions and presenting expansions and results to higher orders (O(L −6 )) than many of those presented in the literature (∼ O(L −2 )). We find good agreement with known results of QNFs for low-lying modes; in the large-ℓ regime, our results are highly consistent with those of Konoplya's 6th-order WKB method.We confirm a universality in the trends of physical features recorded in the literature for the lowlying QNFs (that the real part grows indefinitely, the imaginary tends to a constant as ℓ → ∞, etc.) as we approach large values of ℓ within these spacetimes, and explore the consequent interplay between BH parameters and QNFs in the eikonal limit.

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“…For the Rarita-Schwinger case, L = L + 1/2 = κ = ℓ + 2 = j + 1/2 for ℓ ∈ N o and j = 3/2, 5/2, ... [55][56][57][58].…”

Section: A the Dolan-ottewill Expansion Methodsmentioning

confidence: 99%

“…For maximally-symmetric BH spacetimes, the effective Dirac [35,[51][52][53][54] and Rarita-Schwinger [55][56][57][58] potentials have a supersymmetric form,…”

Section: B Half-integer Spin Perturbationsmentioning

confidence: 99%

Section: B Half-integer Spin Perturbationsmentioning

confidence: 99%

“…We may now turn to Ref. [57], where a study of the spin-3/2 perturbations of higherdimensional RN BHs yielded TT eigenmodes for which the potentials V 1,2 were defined in terms of…”

Section: Spin-3/2 Perturbationsmentioning

confidence: 99%

Section: While Numerical Techniques Have Been Exploited Extensively I...mentioning

confidence: 99%

See 3 more Smart Citations

Quasinormal modes for integer and half-integer spins within the large angular momentum limit

Chen,

Cho,

Chrysostomou

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

Higher order WKB formula for quasinormal modes and grey-body factors: recipes for quick and accurate calculations

Konoplya

Zhidenko

Zinhailo

2019

Class. Quantum Grav.

294

248

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The WKB approach for finding quasinormal modes of black holes, suggested in [1] by Schutz and Will at the first order and later developed to higher orders [2][3][4], became popular during the past decades, because, unlike more sophisticated numerical approaches, it is automatic for different effective potentials and mostly provides sufficient accuracy. At the same time, the seeming simplicity of the WKB approach resulted in appearance of a big number of partially misleading papers, where the WKB formula was used beyond its scope of applicability. Here we review various situations in which the WKB formula can or cannot bring us to reliable conclusions. As the WKB series converges only asymptotically, there is no mathematically strict criterium for evaluation of an error. Therefore, here we are trying to introduce a number of practical recipes instead and summarize cases in which higher WKB orders improve accuracy. We show that averaging of the Padé approximations, suggested first by J. Matyjasek and M. Opala [4], leads to much higher accuracy of the WKB approach, estimate the error and present the automatic code [5] which computes quasinormal modes and grey-body factors. WKB orderPublication 1 B. Mashhoon [8], B. Schutz and C. Will [1] 2-3 S. Iyer and C. Will [2] 4-6 R. Konoplya [3] 7-13 J. Matyjasek and M. Opala [4] 3 0.

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Asymptotic quasinormal frequencies of different spin fields in d-dimensional spherically-symmetric black holes

Chen¹,

Cho²,

Chrysostomou³

et al. 2022

Class. Quantum Grav.

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While Hod's conjecture is demonstrably restrictive, the link he observed between black hole (BH) area quantisation and the large overtone ($n$) limit of quasinormal frequencies (QNFs) motivated intense scrutiny of the regime, from which an improved understanding of asymptotic quasinormal frequencies (aQNFs) emerged. A further outcome was the development of the ``monodromy technique", which exploits an anti-Stokes line analysis to extract physical solutions from the complex plane. Here, we use the monodromy technique to validate extant aQNF expressions for perturbations of integer spin, and provide new results for the aQNFs of half-integer spins within higher-dimensional Schwarzschild, Reissner-Nordstr{\"o}m, and Schwarzschild (anti-)de Sitter BH spacetimes. Bar the Schwarzschild anti-de Sitter case, the spin-1/2 aQNFs are purely imaginary; the spin-3/2 aQNFs resemble spin-1/2 aQNFs in Schwarzschild and Schwarzschild de Sitter BHs, but match the gravitational perturbations for most others. Particularly for Schwarzschild, extremal Reissner-Nordstr{\"o}m, and several Schwarzschild de Sitter cases, the application of $n \rightarrow \infty$ generally fixes $\mathbb{R}e \{ \omega \}$ and allows for the unbounded growth of $\mathbb{I}m \{ \omega \}$ in fixed quantities.

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Quasinormal modes and absorption probabilities of spin- 3/2 fields in D -dimensional Reissner-Nordström black hole spacetimes

Cited by 11 publications

References 16 publications

Quasinormal modes for integer and half-integer spins within the large angular momentum limit

Quasinormal modes for integer and half-integer spins within the large angular momentum limit

Higher order WKB formula for quasinormal modes and grey-body factors: recipes for quick and accurate calculations

Asymptotic quasinormal frequencies of different spin fields in d-dimensional spherically-symmetric black holes

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