pith. sign in

arxiv: 2604.19848 · v2 · pith:QJ73CLYFnew · submitted 2026-04-21 · 🌀 gr-qc · astro-ph.HE· hep-th· quant-ph

Greybody Factor, Resonant Frequencies, and Entropy Quantization of Charged Scalar Fields in the Kerr-EMDA Black Hole

Naz{\i}m Sertkan , \.Izzet Sakall{\i} This is my paper

Pith reviewed 2026-05-25 06:08 UTC · model grok-4.3

classification 🌀 gr-qc astro-ph.HEhep-thquant-ph
keywords Kerr-EMDA black holeconfluent Heun functionsquasinormal modesentropy quantizationgreybody factorcharged scalar fieldsresonant frequenciesMaggiore prescription
0
0 comments X

The pith

Charged scalar perturbations on Kerr-EMDA black holes produce resonant frequencies with imaginary parts spaced exactly by 1/(2M), yielding a horizon-dependent entropy quantum.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper solves the gauge-covariant Klein-Gordon equation for charged massive scalars on the Kerr-EMDA background by separating variables into angular and radial confluent Heun functions. The polynomial termination condition on these functions supplies a discrete resonant frequency spectrum whose imaginary parts differ by the constant 1/(2M). Inserting this spacing into the Maggiore prescription and the first law of black-hole thermodynamics produces the entropy quantum 4π r_+/(r_+ - r_-). The same termination condition also supplies closed-form greybody factors once the fields are taken massless. The resulting entropy spacing reduces to the Schwarzschild value 4π but diverges as the inner and outer horizons coincide.

Core claim

Exact radial solutions for charged scalar fields on the Kerr-EMDA geometry are expressed by confluent Heun functions whose parameters incorporate the electromagnetic coupling q. The requirement that these functions reduce to polynomials fixes the allowed complex frequencies; their imaginary parts form an arithmetic progression with common difference 1/(2M). The Maggiore relation then converts the frequency spacing into an area quantum, and the first law converts that area quantum into the entropy quantum δS_BH = 4π r_+/(r_+ - r_-). In the massless uncharged limit the Heun functions collapse to hypergeometric functions, producing the first closed-form greybody factor for the geometry, which a

What carries the argument

The polynomial termination condition imposed on the confluent Heun function solutions of the radial wave equation.

If this is right

  • The entropy quantum equals 4π when the black hole reduces to Schwarzschild.
  • The entropy quantum diverges as the black hole approaches extremality.
  • The imaginary-part spacing remains fixed by the mass M alone, independent of charge, rotation, or dilaton parameters.
  • In the massless limit the greybody factor is given by a ratio of hypergeometric functions that encodes superradiant amplification.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The same termination technique may produce analogous spacing in other black-hole backgrounds whose wave equations reduce to confluent Heun form.
  • A diverging entropy quantum near extremality could alter thermodynamic stability arguments for near-extremal Kerr-EMDA solutions.
  • Observational bounds on quasinormal-mode spacing could constrain the dilaton parameter once the universal 1/(2M) prediction is tested.

Load-bearing premise

The polynomial termination condition on the confluent Heun functions correctly locates the resonant frequencies to which the Maggiore prescription can be applied.

What would settle it

A high-precision numerical integration of the radial equation for any specific Kerr-EMDA parameters that yields imaginary frequency differences differing from 1/(2M) would falsify the claimed spectrum.

Figures

Figures reproduced from arXiv: 2604.19848 by \.Izzet Sakall{\i}, Naz{\i}m Sertkan.

Figure 1
Figure 1. Figure 1: (a) The function K(r) = ωΣr − am + qQr for several values of the scalar charge q, with M = 1, a = 0.5M, Q = 0.3M, m = 1, and ω = 0.4 M−1 . The dashed vertical line marks the outer horizon r+ ≃ 1.96M. Increasing q raises K due to the positive qQr contribution, with the curves merging near r ≈ 0 where K → a 2ω − am ≃ −0.4. (b) The superradiant bound ωc = mΩH − qΦH as a function of q for different BH spins at… view at source ↗
Figure 2
Figure 2. Figure 2: (a) Entropy quantum δSBH/π as a function of the spin parameter a/M for Q = 0 (Kerr, black), Q = 0.3M (red), and Q = 0.6M (green). The horizontal dashed line marks δSBH = 2π. All curves start near 4π (Schwarzschild value) at a = 0 and diverge at the respective extremal limits a = M + D, where δr → 0 and TH → 0. The dilaton shift D = Q2/(2M) extends the extremal spin beyond M (e.g. amax = 1.045M for Q = 0.3M… view at source ↗
Figure 3
Figure 3. Figure 3: Effective potential Veff(r) for massless uncharged scalars on the Kerr-EMDA background with M = 1 and ω = 0.5 M−1 . (a) Veff for ℓ = 0, 1, 2 at fixed a = 0.5M, Q = 0.3M, m = 0: higher ℓ produces a deeper well and taller centrifugal barrier. (b) Veff for Q = 0.01M (near-Kerr), 0.3M, 0.6M at fixed a = 0.5M, ℓ = 1: increasing Q (and hence the dilaton parameter D) lowers the barrier minimum and shifts the peak… view at source ↗
Figure 4
Figure 4. Figure 4: s-wave (ℓ = 0, m = 0) greybody factor Γ0(ω) for the Kerr-EMDA BH with a = 0.5M, showing the dilaton effect for Q = 0.1M (D = 0.005M), 0.3M (D = 0.045M), and 0.6M (D = 0.180M). (a) Full range: all curves saturate to unity at high frequencies. (b) Zoomed to ωM ∈ [0.15, 0.25]: increasing D enhances Γ0 at low energies, confirming that the dilaton-broadened barrier is more transparent. of Γ0 toward unity, while… view at source ↗
Figure 5
Figure 5. Figure 5: s-wave (ℓ = 0, m = 0) greybody factor Γ0(ω) for the Kerr-EMDA BH with Q = 0.3M, showing the spin effect for a = 0.1M, 0.3M, 0.5M, and 0.8M. (a) Full range: all curves approach unity at high frequencies. (b) Zoomed to ωM ∈ [0.15, 0.25]: higher spin produces a larger GF, consistent with a thinner effective potential barrier [PITH_FULL_IMAGE:figures/full_fig_p026_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Partial wave hierarchy of the greybody factor Γ [PITH_FULL_IMAGE:figures/full_fig_p026_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Hawking radiation from the Kerr-EMDA BH with [PITH_FULL_IMAGE:figures/full_fig_p030_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Normalized absorption cross-section σabs/AH versus ωM, summed over ℓ = 0, 1, 2, 3 with a = 0.5M and m = 0, for Q = 0.1M, 0.3M, and 0.6M. The horizontal dotted line marks σabs = AH. All curves approach unity as ω → 0, verifying the low-energy universality. The oscillatory structure at intermediate energies reflects partial wave interference, with the pattern depending on the dilaton parameter D. 8 Special L… view at source ↗
read the original abstract

We study charged massive scalar field perturbations on the rotating black hole (BH) background of Einstein-Maxwell-Dilaton-Axion (EMDA) theory, known as the Kerr-EMDA BH. Starting from the gauge-covariant Klein-Gordon equation (KGE), we perform a full separation of variables and obtain exact analytical solutions for both the angular and radial parts in terms of confluent Heun functions (CHFs). Unlike the earlier neutral scalar treatment by Senjaya and Ponglertsakul [Eur. Phys. J. C \textbf{85}, 352 (2025)], the electromagnetic coupling $q$ fundamentally alters the structure of the Heun parameters and produces qualitatively new physics. Applying the CHF polynomial condition, we derive the resonant frequency spectrum whose imaginary parts are equispaced with $|\Delta\omega_I| = 1/(2M)$, a universal spacing determined solely by the BH mass. Via the Maggiore prescription and the first law of BH thermodynamics, this yields a parameter-dependent entropy quantum $\delta S_{\text{BH}} = 4\pi r_+/(r_+ - r_-)$, which reduces to $4\pi$ for Schwarzschild but diverges at extremality -- {\color{black}in contrast to the universal $2\pi$ obtained for the rotating linear dilaton BH (RLDBH).} We construct the effective potential governing scalar wave scattering and analyze its dependence on the dilaton parameter $D$, rotation $a$, and scalar charge $q$. In the massless uncharged limit, the CHF reduces to the Gauss hypergeometric function, {\color{black}enabling us to compute the first analytical greybody factor (GF) for the Kerr-EMDA geometry; we show that this reduction extends to massless charged scalars, yielding a closed-form GF that captures superradiant amplification.} We examine how the dilaton deformation distinguishes the Kerr-EMDA spectrum from the standard Kerr and Kerr-Newman cases.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 2 minor

Summary. The manuscript analyzes charged massive scalar perturbations on the Kerr-EMDA black hole. It obtains exact separated solutions in confluent Heun functions for the angular and radial equations, applies the CHF polynomial termination condition to extract a resonant frequency spectrum with equispaced imaginary parts satisfying |Δω_I| = 1/(2M), invokes the Maggiore prescription together with the first law to obtain the entropy quantum δS_BH = 4π r_+/(r_+ - r_-), and derives closed-form greybody factors in the massless limit by reduction to hypergeometric functions.

Significance. If the spectral condition were valid, the work would supply the first analytical greybody factors and an explicit parameter-dependent entropy quantization for charged scalars in this dilaton-axion geometry, extending the neutral case and distinguishing it from Kerr and Kerr-Newman. The claimed universal mass-only spacing and its thermodynamic consequences would constitute a concrete, falsifiable prediction.

major comments (1)
  1. [Abstract and resonant-frequency derivation] Abstract and the section deriving resonant frequencies via the CHF polynomial condition: the termination condition produces |Δω_I| = 1/(2M). In the Schwarzschild limit (D = a = q = 0) this yields twice the established asymptotic spacing Im(ω_n) ≈ −(n + 1/2)/(4M). The discrepancy indicates that the polynomial condition does not enforce the correct outgoing-wave boundary condition at infinity required for physical quasinormal modes; consequently the derived δS_BH = 4π (instead of the 2π obtained from the correct spacing) and its EMDA generalization rest on an invalid spectral condition.
minor comments (2)
  1. [Abstract] The contrast with the RLDBH result (universal 2π) is stated but the origin of the numerical factor difference is not traced to the specific boundary-condition implementation.
  2. [Separation of variables] Notation for the electromagnetic coupling q and its appearance in the Heun parameters should be cross-referenced to the separated radial equation for clarity.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the careful reading of our manuscript and for identifying a substantive issue with the resonant-frequency derivation. We respond to the major comment below and indicate the revisions that will be made.

read point-by-point responses

  1. Referee: [Abstract and resonant-frequency derivation] Abstract and the section deriving resonant frequencies via the CHF polynomial condition: the termination condition produces |Δω_I| = 1/(2M). In the Schwarzschild limit (D = a = q = 0) this yields twice the established asymptotic spacing Im(ω_n) ≈ −(n + 1/2)/(4M). The discrepancy indicates that the polynomial condition does not enforce the correct outgoing-wave boundary condition at infinity required for physical quasinormal modes; consequently the derived δS_BH = 4π (instead of the 2π obtained from the correct spacing) and its EMDA generalization rest on an invalid spectral condition.

    Authors: We agree with the referee that the polynomial termination condition on the confluent Heun functions does not enforce the outgoing-wave boundary condition at infinity. This is directly confirmed by the factor-of-two mismatch with the accepted Schwarzschild asymptotic spacing of the imaginary parts. Consequently the extracted spectrum cannot be identified with physical quasinormal modes, and the subsequent application of the Maggiore prescription to obtain δS_BH = 4π r_+/(r_+ - r_-) is not justified. In the revised manuscript we will remove all claims concerning resonant frequencies, the Maggiore prescription, and the associated entropy quantization from the abstract, introduction, and relevant sections. The exact separated solutions in confluent Heun functions, the effective-potential analysis, and the closed-form greybody factors obtained in the massless limit (via reduction to hypergeometric functions) remain valid and will be retained. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation proceeds from standard CHF termination condition

full rationale

The paper derives the resonant frequencies by applying the polynomial termination condition to the confluent Heun function solutions of the separated radial equation. This is a direct mathematical constraint on the parameters (including frequency ω) that produces the claimed equispacing |Δω_I| = 1/(2M) as an output rather than an input. The subsequent application of the Maggiore prescription and first law to obtain δS_BH is an interpretive step using external literature, not a reduction of the result to a fitted parameter or self-citation within the paper. No load-bearing step reduces by construction to the target entropy quantum or frequency spacing; the chain remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on the validity of the EMDA metric as a known solution, the gauge-covariant Klein-Gordon equation in curved spacetime, and the mathematical termination condition for confluent Heun functions; no new free parameters are introduced in the perturbation analysis itself.

axioms (2)
  • domain assumption Separation of variables applies to the gauge-covariant Klein-Gordon equation on the Kerr-EMDA background.
    Standard assumption in black hole perturbation theory invoked for the angular-radial split.
  • standard math Confluent Heun functions admit polynomial solutions under specific parameter conditions that correspond to physical resonances.
    Mathematical property of the special functions used for exact solutions.

pith-pipeline@v0.9.0 · 5915 in / 1588 out tokens · 74913 ms · 2026-05-25T06:08:29.259538+00:00 · methodology

Review history (2 revisions) →

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

39 extracted references · 39 canonical work pages

  1. [1]

    Release 1.1.12

    NIST Digital Library of Mathematical Functions.https://dlmf.nist.gov/, 2023. Release 1.1.12

    work page 2023

  2. [2]

    Photon spheres, gravitational lensing/mirroring, and grey- body radiation in deformed AdS-Schwarzschild black holes with phantom global monopole.Phys

    Faizuddin Ahmed, Ahmad Al-Badawi, and ˙Izzet Sakallı. Photon spheres, gravitational lensing/mirroring, and grey- body radiation in deformed AdS-Schwarzschild black holes with phantom global monopole.Phys. Dark Univ., 49: 101988, 2025. doi: 10.1016/j.dark.2025.101988

    work page doi:10.1016/j.dark.2025.101988 2025

  3. [3]

    Greybody radiation of scalar and Dirac perturbations of NUT black holes.Eur

    Ahmad Al-Badawi, Sara Kanzi, and ˙Izzet Sakallı. Greybody radiation of scalar and Dirac perturbations of NUT black holes.Eur. Phys. J. Plus, 137(1):94, 2022. doi: 10.1140/epjp/s13360-021-02227-9

    work page doi:10.1140/epjp/s13360-021-02227-9 2022

  4. [4]

    Fermionic and bosonic greybody factors as well as quasinormal modes for charged Taub NUT black holes.Annals Phys., 452:169294, 2023

    Ahmad Al-Badawi, Sara Kanzi, and ˙Izzet Sakallı. Fermionic and bosonic greybody factors as well as quasinormal modes for charged Taub NUT black holes.Annals Phys., 452:169294, 2023. doi: 10.1016/j.aop.2023.169294

    work page doi:10.1016/j.aop.2023.169294 2023

  5. [5]

    Regular magnetically charged black holes from nonlinear elec- trodynamics: Thermodynamics, light deflection, and orbital dynamics.Phys

    Ekrem Aydiner, Erdem Sucu, and ˙Izzet Sakallı. Regular magnetically charged black holes from nonlinear elec- trodynamics: Thermodynamics, light deflection, and orbital dynamics.Phys. Dark Univ., 50:102164, 2025. doi: 10.1016/j.dark.2025.102164

    work page doi:10.1016/j.dark.2025.102164 2025

  6. [6]

    Bekenstein

    Jacob D. Bekenstein. The quantum mass spectrum of the Kerr black hole.Lett. Nuovo Cim., 11:467–470, 1974. doi: 10.1007/BF02762768. URLhttps://doi.org/10.1007/BF02762768

    work page doi:10.1007/bf02762768 1974

  7. [7]

    Starinets

    Emanuele Berti, Vitor Cardoso, and Andrei O. Starinets. Quasinormal modes of black holes and black branes. Class. Quant. Grav., 26:163001, 2009. doi: 10.1088/0264-9381/26/16/163001. URLhttps://doi.org/10.1088/ 0264-9381/26/16/163001

    work page doi:10.1088/0264-9381/26/16/163001 2009

  8. [8]

    Bonelli, C

    G. Bonelli, C. Iossa, D. Lichtig, and A. Tanzini. Exact solution of kerr black hole perturbations via cft2 and instanton counting.Phys. Rev. D, 105:044047, 2022. doi: 10.1103/PhysRevD.105.044047

    work page doi:10.1103/physrevd.105.044047 2022

  9. [9]

    Notes Phys.Springer, 2015

    Richard Brito, Vitor Cardoso, and Paolo Pani.Superradiance: New Frontiers in Black Hole Physics, volume 906 ofLect. Notes Phys.Springer, 2015. doi: 10.1007/978-3-319-19000-6. URLhttps://doi.org/10.1007/ 978-3-319-19000-6. 36

    work page doi:10.1007/978-3-319-19000-6 2015

  10. [10]

    Cardoso, A

    V. Cardoso, A. S. Miranda, E. Berti, H. Witek, and V. T. Zanchin. Geodesic stability, lyapunov exponents and quasinormal modes.Phys. Rev. D, 79:064016, 2009. doi: 10.1103/PhysRevD.79.064016

    work page doi:10.1103/physrevd.79.064016 2009

  11. [11]

    Creek, O

    S. Creek, O. Efthimiou, P. Kanti, and K. Tamvakis. Greybody factors for brane scalar fields in a rotating black hole background.Phys. Rev. D, 75:084043, 2007. doi: 10.1103/PhysRevD.75.084043

    work page doi:10.1103/physrevd.75.084043 2007

  12. [12]

    Das, Gary Gibbons, and Samir D

    Sumit R. Das, Gary Gibbons, and Samir D. Mathur. Universality of low-energy absorption cross-sections for black holes.Phys. Rev. Lett., 78:417–419, 1997. doi: 10.1103/PhysRevLett.78.417. URLhttps://doi.org/10.1103/ PhysRevLett.78.417

    work page doi:10.1103/physrevlett.78.417 1997

  13. [13]

    Fernando

    S. Fernando. Greybody factors of charged dilaton black holes in 2+1 dimensions.Gen. Rel. Grav., 37:461–481, 2005. doi: 10.1007/s10714-005-0035-x

    work page doi:10.1007/s10714-005-0035-x 2005

  14. [14]

    P. P. Fiziev. Classes of exact solutions to the Teukolsky master equation.Class. Quant. Grav., 27:135001, 2010. doi: 10.1088/0264-9381/27/13/135001. URLhttps://doi.org/10.1088/0264-9381/27/13/135001

    work page doi:10.1088/0264-9381/27/13/135001 2010

  15. [15]

    Class of stationary axisymmetric solutions of the Einstein- Maxwell-dilaton-axion field equations.Phys

    Alberto Garcia, Dmitri Galtsov, and Oleg Kechkin. Class of stationary axisymmetric solutions of the Einstein- Maxwell-dilaton-axion field equations.Phys. Rev. Lett., 74:1276–1279, 1995. doi: 10.1103/PhysRevLett.74.1276. URLhttps://doi.org/10.1103/PhysRevLett.74.1276

    work page doi:10.1103/physrevlett.74.1276 1995

  16. [16]

    Horowitz, and Andrew Strominger

    David Garfinkle, Gary T. Horowitz, and Andrew Strominger. Charged black holes in string theory.Phys. Rev. D, 43:3140–3143, 1991. doi: 10.1103/PhysRevD.43.3140. URLhttps://doi.org/10.1103/PhysRevD.43.3140

    work page doi:10.1103/physrevd.43.3140 1991

  17. [17]

    S. G. Ghosh and R. K. Walia. Rotating black holes in einstein-maxwell-dilaton-axion gravity.Ann. Phys., 434:168612,

    work page

  18. [18]

    doi: 10.1016/j.aop.2021.168619

    work page doi:10.1016/j.aop.2021.168619 2021

  19. [19]

    G. W. Gibbons and Kei-ichi Maeda. Black Holes and Membranes in Higher Dimensional Theories with Dilaton Fields.Nucl. Phys. B, 298:741–775, 1988. doi: 10.1016/0550-3213(88)90006-5. URLhttps://doi.org/10.1016/ 0550-3213(88)90006-5

    work page doi:10.1016/0550-3213(88)90006-5 1988

  20. [20]

    Greybody Factors for d-Dimensional Black Holes.Adv

    Troels Harmark, Jose Natario, and Ricardo Schiappa. Greybody Factors for d-Dimensional Black Holes.Adv. Theor. Math. Phys., 14(3):727–794, 2010. doi: 10.4310/ATMP.2010.v14.n3.a1. URLhttps://doi.org/10.4310/ATMP. 2010.v14.n3.a1

    work page doi:10.4310/atmp.2010.v14.n3.a1 2010

  21. [21]

    S. W. Hawking. Particle Creation by Black Holes.Commun. Math. Phys., 43:199–220, 1975. doi: 10.1007/BF02345020. URLhttps://doi.org/10.1007/BF02345020

    work page doi:10.1007/bf02345020 1975

  22. [22]

    A. Higuchi. Low frequency scalar absorption cross-sections for stationary black holes.Class. Quant. Grav., 18: L139–L143, 2001. doi: 10.1088/0264-9381/18/20/102. 37

    work page doi:10.1088/0264-9381/18/20/102 2001

  23. [23]

    Bohr’s correspondence principle and the area spectrum of quantum black holes.Phys

    Shahar Hod. Bohr’s correspondence principle and the area spectrum of quantum black holes.Phys. Rev. Lett., 81: 4293, 1998. doi: 10.1103/PhysRevLett.81.4293. URLhttps://doi.org/10.1103/PhysRevLett.81.4293

    work page doi:10.1103/physrevlett.81.4293 1998

  24. [24]

    Greybody radiation and quasinormal modes of Kerr-like black hole in Bumblebee gravity model.Eur

    Sara Kanzi and ˙Izzet Sakallı. Greybody radiation and quasinormal modes of Kerr-like black hole in Bumblebee gravity model.Eur. Phys. J. C, 81(6):501, 2021. doi: 10.1140/epjc/s10052-021-09299-y

    work page doi:10.1140/epjc/s10052-021-09299-y 2021

  25. [25]

    R. A. Konoplya and Alexander Zhidenko. Quasinormal modes of black holes: From astrophysics to string theory.Rev. Mod. Phys., 83:793–836, 2011. doi: 10.1103/RevModPhys.83.793. URLhttps://doi.org/10.1103/RevModPhys. 83.793

    work page doi:10.1103/revmodphys.83.793 2011

  26. [26]

    d-dimensional black hole entropy spectrum from quasinormal modes.Phys

    Gabor Kunstatter. d-dimensional black hole entropy spectrum from quasinormal modes.Phys. Rev. Lett., 90:161301,

    work page

  27. [27]

    doi: 10.1103/PhysRevLett.90.161301

    work page doi:10.1103/physrevlett.90.161301

  28. [28]

    Physical interpretation of the spectrum of black hole quasinormal modes.Phys

    Michele Maggiore. Physical interpretation of the spectrum of black hole quasinormal modes.Phys. Rev. Lett., 100: 141301, 2008. doi: 10.1103/PhysRevLett.100.141301. URLhttps://doi.org/10.1103/PhysRevLett.100.141301

    work page doi:10.1103/physrevlett.100.141301 2008

  29. [29]

    Don N. Page. Particle Emission Rates from a Black Hole: Massless Particles from an Uncharged, Nonrotating Hole. Phys. Rev. D, 13:198–206, 1976. doi: 10.1103/PhysRevD.13.198. URLhttps://doi.org/10.1103/PhysRevD.13. 198

    work page doi:10.1103/physrevd.13.198 1976

  30. [30]

    Ronveaux.Heun’s Differential Equations

    A. Ronveaux.Heun’s Differential Equations. Oxford University Press, Oxford, 1995

    work page 1995

  31. [31]

    Sakallı and S

    ˙I. Sakallı and S. Kanzi. Topical review: greybody factors and quasinormal modes for black holes in various theories — fingerprints of invisibles.Turk. J. Phys., 46:51–103, 2022. doi: 10.55730/1300-0101.2691

    work page doi:10.55730/1300-0101.2691 2022

  32. [32]

    Analytical solutions in rotating linear dilaton black holes: resonant frequencies, quantization, greybody factor, and Hawking radiation.Phys

    ˙Izzet Sakallı. Analytical solutions in rotating linear dilaton black holes: resonant frequencies, quantization, greybody factor, and Hawking radiation.Phys. Rev. D, 94(8):084040, 2016. doi: 10.1103/PhysRevD.94.084040. URLhttps: //doi.org/10.1103/PhysRevD.94.084040

    work page doi:10.1103/physrevd.94.084040 2016

  33. [33]

    Analytical solutions in a cosmic string Born–Infeld-dilaton black hole geometry: quasinormal modes and quantization.Gen

    ˙Izzet Sakallı, Kimet Jusufi, and Ali ¨Ovg¨ un. Analytical solutions in a cosmic string Born–Infeld-dilaton black hole geometry: quasinormal modes and quantization.Gen. Rel. Grav., 50:125, 2018. doi: 10.1007/s10714-018-2455-4

    work page doi:10.1007/s10714-018-2455-4 2018

  34. [34]

    Rotating charged black hole solution in heterotic string theory.Phys

    Ashoke Sen. Rotating charged black hole solution in heterotic string theory.Phys. Rev. Lett., 69:1006–1009, 1992. doi: 10.1103/PhysRevLett.69.1006. URLhttps://doi.org/10.1103/PhysRevLett.69.1006

    work page doi:10.1103/physrevlett.69.1006 1992

  35. [35]

    The spectroscopy of Kerr-Einstein-Maxwell-dilaton-axion: exact qua- sibound states, scalar cloud, horizon’s Boson statistics and superradiant.Eur

    David Senjaya and Supakchai Ponglertsakul. The spectroscopy of Kerr-Einstein-Maxwell-dilaton-axion: exact qua- sibound states, scalar cloud, horizon’s Boson statistics and superradiant.Eur. Phys. J. C, 85(3):352, 2025. doi: 10.1140/epjc/s10052-025-14014-2. URLhttps://doi.org/10.1140/epjc/s10052-025-14014-2

    work page doi:10.1140/epjc/s10052-025-14014-2 2025

  36. [36]

    Investigating the Generalized Uncertainty Principle Effects on Hawking Radiation in Rotating Linear Dilaton Black Holes

    Erdem Sucu. Investigating the Generalized Uncertainty Principle Effects on Hawking Radiation in Rotating Linear Dilaton Black Holes. 2024. 38

    work page 2024

  37. [37]

    Exploring Lorentz-violating effects of Kalb-Ramond field on charged black hole thermodynamics and photon dynamics.Phys

    Erdem Sucu and ˙Izzet Sakallı. Exploring Lorentz-violating effects of Kalb-Ramond field on charged black hole thermodynamics and photon dynamics.Phys. Rev. D, 111(6):064049, 2025. doi: 10.1103/PhysRevD.111.064049

    work page doi:10.1103/physrevd.111.064049 2025

  38. [38]

    Quantum-corrected thermodynamics and plasma lensing in non-minimally coupled symmetric teleparallel black holes.Phys

    Erdem Sucu, ˙Izzet Sakallı, ¨Ozcan Sert, and Yusuf Sucu. Quantum-corrected thermodynamics and plasma lensing in non-minimally coupled symmetric teleparallel black holes.Phys. Dark Univ., 50:102063, 2025. doi: 10.1016/j.dark. 2025.102063

    work page doi:10.1016/j.dark 2025

  39. [39]

    H. S. Vieira. Quasibound states, stability and wave functions of the test fields in the consistent 4D Einstein- Gauss-Bonnet gravity.Universe, 9(5):205, 2023. doi: 10.3390/universe9050205. URLhttps://doi.org/10.3390/ universe9050205. 39

    work page doi:10.3390/universe9050205 2023