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REVIEW 3 major objections 4 minor 57 references

Exact Dynamical Black Hole Solutions in Five or Higher Dimensions

T0 review · 3 major / 4 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read The paper constructs new exact, time-dependent solutions to Einstein-Maxwell-dilaton gravity in D ≥ 5 dimensions on a Bianchi type IX base space, solving the full field equations in three coupling regimes.

desk verdict Honest and checkable exact-solution work in D≥5, but the 'black hole' label is not earned because no horizon is ever located. read the letter →

arxiv 2501.07495 v1 pith:GDB5UGMM submitted 2025-01-13 gr-qc hep-th

B. H. Fahim , A. M. Ghezelbash This is my paper · ORCID
classification gr-qchep-th MSC 83C5783C1583E15 PACS 04.20.Jb04.70.Bw04.50.Gh
keywords exactsolutionsdynamicalblackholesEinstein-Maxwell-dilatontheoryBianchitypeIXcosmologicalconstanthigher-dimensionalgravityKastor-Traschendimensionaluplift
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper constructs new exact, time-dependent solutions to Einstein-Maxwell-dilaton gravity in five or more spacetime dimensions. Working on a Bianchi type IX base space and allowing two independent coupling constants for the dilaton to the Maxwell field and the cosmological constant, the authors solve the full field equations analytically in three distinct coupling regimes. The resulting metrics are non-stationary and, depending on parameters, asymptotically de Sitter, anti-de Sitter, or flat. The authors identify the solutions as dynamical black holes and show that some of them uplift to higher-dimensional Einstein-form or Einstein-Maxwell theories. If correct, the work provides new exact dynamical black holes beyond the known Kastor-Traschen family.

What carries the argument

The construction rests on a three-part ansatz: a metric that separates time-dependence into a factor R(t)^2 multiplying a spatial part built from the four-dimensional Bianchi type IX geometry (a homogeneous three-sphere-like space with SU(2) isometry described by Maurer-Cartan one-forms), with a conformal factor $H^{{-2}}$ in front of $dt^{2}$; a dilaton that is a logarithm of H and R; and a Maxwell gauge field proportional to R^X H^Y. Substituting these ansatzes into the field equations reduces them to constraints that determine H, R, the dilaton, the gauge field, the coupling-constant relation, and the cosmological constant.

What would settle it

Look for a trapped surface or compute whether the hypersurface H=0 is a null surface in the N=4 metric (14); if the outgoing null expansion never becomes negative, these are not black holes.

Watch

Extended reading notes

Core claim

The central claim is that the metrics (14), (40), and (54), together with the accompanying dilaton and Maxwell fields, solve the full field equations of the N+1-dimensional Einstein-Maxwell-dilaton action (13) with arbitrary cosmological constant, for any N ≥ 4, in three regimes: non-equal coupling constants ab = -(N-2), equal non-zero couplings a = b, and vanishing couplings (Einstein-Maxwell). The key results include explicit forms H(r,θ) = (g_+ $r^{2}$ cosθ + g_-)^{(N-2)/($a^{2}$+N-2)}, R(t) = (ηt+ν)^{$a^{2}$/(N-2)^2}, and the dilaton and electric field expressions, along with constraints on the cosmological constant that allow it to be positive, zero, or negative. These solutions are almost conformally regular everywhere and, the authors argue, describe dynamical black holes in D ≥ 5 dimensions, generalizing Kastor-Traschen-like time-dependent charged black holes to higher dimensions on a Bianchi IX base.

Load-bearing premise

The spacetimes are called black holes, but the paper never computes an event or apparent horizon; if no horizon exists, the curvature singularities would be naked and the central black-hole claim would fail.

Editorial extensions

If this is right

  • If the solutions are exact, they provide the first fully explicit dynamical black hole metrics in Einstein-Maxwell-dilaton theory in arbitrary dimension D ≥ 5, beyond the known Kastor-Traschen family.
  • The cosmological constant can be positive, zero, or negative depending on the dimension N and coupling a, so the same ansatz yields asymptotically de Sitter, flat, and anti-de Sitter examples.
  • For special coupling values, the solutions lift to higher-dimensional Einstein-form or Einstein-Maxwell theories with a fixed internal dimension, showing a direct link between the dilaton coupling and the compactification scale.
  • Because the results are independent of the Bianchi type IX parameters k and c, the solutions hold on every sub-geometry of that base space, including Eguchi-Hanson-type cases.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A natural next test is whether the hypersurface H=0 is a null or Killing horizon; if it is not, these exact solutions would be naked singularities, a distinction the paper does not settle.
  • The same ansatz may work on other self-dual base manifolds with SU(2) structure, so the construction could be extended to generate more dynamical charged solutions without new integration work.
  • If the asymptotically AdS cases are used as holographic backgrounds, the computed c-function suggests testable RG-flow behavior; a direct holographic entanglement-entropy calculation could confirm the UV/IR interpretation.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The paper constructs three families of exact solutions to N+1-dimensional Einstein-Maxwell-dilaton theory with two coupling constants and a cosmological constant, using a Bianchi type IX base metric. For the cases of (i) unequal couplings, (ii) equal nonzero couplings, and (iii) zero couplings, the paper gives the metric ansatze (14), (40), and (54), solves the field equations for H, R, the dilaton, and the Maxwell field, computes curvature invariants, electric fields, and c-functions, and discusses uplifts to higher-dimensional theories. The title and conclusions claim that these are new dynamical black hole solutions in D ≥ 5 dimensions.

Significance. If the algebraic verification is correct, the paper provides a useful set of exact time-dependent solutions in a well-motivated theory, with explicit constraints on the coupling constants and cosmological constant. The derivation is self-contained: the authors substitute their ansatze into the full field equations and report the resulting consistency conditions, including the lengthy Mt equation in the appendix. The claimed embeddings into higher-dimensional Einstein-form and Einstein-Maxwell theories are also explicit, with sample values checked. However, the physical interpretation as black holes is not established, and the statement that a specialization is made 'with no loss of generality' is unjustified. These points must be addressed before the central claim can be accepted.

major comments (3)
  1. [Sections II–IV and VI] The black-hole claim is unsupported because no horizon is located. In all three families the time-time metric component is g_tt = -1/H^2, with H given by (26), (43), and (56), respectively; hence g_tt has no zero at any finite regular surface. The surfaces H=0 are curvature singularities according to the invariants (32)–(33), and the paper does not show that they are shielded by an apparent horizon or a trapped surface. Without such a calculation, the solutions may be naked singularities, and the conclusion that they are 'dynamical black holes' is not justified. The authors should either compute the apparent/event horizon for these spacetimes or revise the title, abstract, and conclusions to claim exact dynamical solutions rather than black holes.
  2. [Section III, Eq. (48)] The phrase 'we consider p=a^2+2 with no loss of generality' is not justified. In the solution (43), p is an arbitrary constant that enters through the relation p=(N-2)Δ+1/Δ with R(t)=(ηt+ν)^Δ. Setting p=a^2+2 fixes Δ=1/(a^2+4-N) and discards other branches of the solution family. Unless the authors show a coordinate redefinition or a field redefinition that absorbs p, this is a genuine specialization and not a lossless choice. This restriction propagates to the cosmological constant expression (47) and to the subsequent physical discussion, so it should be stated explicitly as a restriction.
  3. [Section IV, Eq. (60)] The statement 'Assuming p=1' is likewise a specialization rather than a general choice. The constant p first appears in the metric function (56), and setting p=1 fixes Y=-(N-2) as in (60). The authors note that this reproduces the five-dimensional results of Ref. [50], but the general family with arbitrary p is not presented. Please clarify whether the solutions for all p are valid and, if so, state the general expressions or explicitly label the p=1 case as a particular subclass used for comparison with previous work.
minor comments (4)
  1. [Abstract and Introduction] The term 'almost conformally regular everywhere' is used without a definition. Please define what is meant by this property or remove the phrase.
  2. [Figure 2 caption] The caption for panel (b) says 'in terms of N for two different values of a', but the text and axis indicate the plot is in terms of the coupling constant a for two values of N. Please correct the caption.
  3. [Throughout] The notation for the dilaton field alternates between ϕ in the action and Φ for the explicit solutions. Please unify the notation for clarity.
  4. [Conclusions] The statement that the solutions are 'completely unique and analytical' overstates what is shown: the uniqueness applies only within the chosen ansatze, not among all possible solutions. Please rephrase to avoid an unsupported uniqueness claim.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the exact solutions are derived by direct substitution and solving of the field equations from explicit ansatzes; the only self-citation is a non-load-bearing specialization.

full rationale

The paper's derivation chain is self-contained. Starting from the action (13), the authors propose explicit ansatzes for the metric (14), (40), (54), the dilaton (18), (42), and the Maxwell field (19), (41), (55). They then substitute these into the Einstein, Maxwell, and dilaton field equations (15)-(17) and solve for the unknown constants and functions. The constraints such as X+V=2-N (eq. 21), UV=-4a^2 (eq. 23), U=2a^2/(N-2), V=-2(N-2), X=N-2, and ab=-(N-2) (eq. 29) are derived from the equations, not imposed to fit a target solution. The metric functions H(r,theta), R(t), and the cosmological constant Lambda are obtained by solving the resulting differential equations (eqs. 26-28, 43, 46-47, 56-57). No fitted parameter is renamed as a prediction, and no central claim reduces by definition to an input. The only self-referential element is the statement 'In order to reproduce the same results of the reference [50] ... we consider p = a^2+2 with no loss of generality' (Section III). Reference [50] is prior work by the same authors, and this choice specializes a free parameter to match a known five-dimensional solution; it is a restriction used to exhibit a subfamily, not an input that forces the derived field equations or the main exact-solution result. The paper's failure to compute an event or apparent horizon before calling the spacetimes 'dynamical black holes' is a physical-interpretation or correctness concern, not a circularity of the derivation. The exact-solution claim is independently checkable by substitution into the field equations, so the circularity score is 0.

Assumptions & free parameters 6 free parameters · 6 assumptions · 2 invented entities

The central claim rests on standard background mathematics (Bianchi IX geometry and Jacobi elliptic function solutions), the field equations of Einstein-Maxwell-dilaton theory, and the validity of the adopted ansatze. The ansatze are explicit assumptions, and the paper's 'no loss of generality' p choices are ad hoc specializations. No new physical entities are proposed; the extra-dimensional uplifts are standard Kaluza-Klein constructions with no independent observational evidence.

free parameters (6)
  • a
    Dilaton coupling to the Maxwell field in action (13). It is a free theory parameter, constrained in class I by ab=-(N-2), and chosen by hand in figures.
  • b
    Dilaton coupling to the cosmological constant in action (13). Constrained by ab=-(N-2) in class I; equal to a in class II; zero in class III.
  • g+ and g-
    Arbitrary integration constants in H(r,theta). Together they determine the sign of H and hence where curvature singularities at H=0 occur.
  • eta and nu
    Integration constants in the time-dependent scale factor R(t). The conditions eta>=0 and nu>0 are imposed to keep R(t) from vanishing.
  • p = a^2+2 (class II), 1 (class III)
    Exponent introduced in H(t,r,theta). It is arbitrary and related to Delta by p=(N-2)Delta+1/Delta, but the paper fixes it to reproduce earlier results, which is a specialization.
  • k and c
    Parameters of the Bianchi IX base geometry. The authors state the final results are independent of them, so they do not affect the central derivation.
assumptions (6)
  • standard math The Bianchi type IX line element (1) with f,h,g given by equations (8)-(10) satisfies the vacuum Einstein equations and the self-duality conditions.
    Quoted from references [37,38], not rederived in this paper.
  • standard math The field equations (15)-(17) are the correct Euler-Lagrange equations for the action (13).
    Standard variation of the action; cited to [43].
  • domain assumption The metric and matter ansatze (14), (18), (19) and their analogues in Sections III and IV are sufficiently general to capture a genuine black hole solution.
    The paper postulates these forms and verifies consistency, but does not derive them from a more general symmetry principle.
  • domain assumption The coordinate restriction r >= 2c preserves positive definiteness of the spatial Bianchi IX metric (11).
    Stated in Section II immediately after equation (11); used implicitly in all subsequent field equation manipulations.
  • ad hoc to paper The choices p=a^2+2 (class II) and p=1 (class III) are 'with no loss of generality'.
    These specializations of the arbitrary constant p are not forced by the field equations and are introduced to match earlier five-dimensional solutions [50].
  • standard math The dimensional reduction formulas (66)-(70) of [52] apply to the present solutions.
    The uplifting analysis in Section V relies on these cited reduction formulas.
invented entities (2)
  • Internal space of dimension q = (N-1)/(b^2 - 1) in the uplift to a D-dimensional Einstein-form theory
    purpose: Used in Section V to embed the a != b solutions of Section II into a higher-dimensional gravity theory with a form field and no cosmological constant.
    This is a formal Kaluza-Klein internal space derived from the consistency relations (75)-(78). No physical or observational evidence for such an internal dimension is provided, and the paper does not claim it as a prediction.
  • D = 3a^2/(1-a^2) extra Euclidean dimensions in the uplift to Einstein-Maxwell theory with cosmological constant
    purpose: Used in Section III to embed the a=b solutions into a higher-dimensional Einstein-Maxwell theory with a cosmological constant, valid for a in [1/2,1).
    Standard uplift construction from [49], checked explicitly for a=1/2, sqrt(2/5), and 1/sqrt(2). It has no independent experimental handle and is a mathematical tool.

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Pith. "Pith review of Exact Dynamical Black Hole Solutions in Five or Higher Dimensions." pith.science (2026). https://pith.science/paper/GDB5UGMM

@misc{pith2026250107495,
  author       = {Pith},
  title        = {Pith review of: Exact Dynamical Black Hole Solutions in Five or Higher Dimensions},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GDB5UGMM}},
  note         = {Machine review of arXiv:2501.07495}
}
read the original abstract

We construct new classes of the dynamical black hole solutions in five or higher dimensional Einstein-Maxwell theory, coupled to a dilaton field, in the presence of arbitrary cosmological constant. The dilaton field interacts non-trivially with the Maxwell field, as well as the cosmological constant, with two arbitrary coupling constants. The solutions are non-stationary, and almost conformally regular everywhere. To construct the solutions, we use the four-dimensional Bianchi type IX geometry, as the base space. We find three different classes of solutions, based on the values of the coupling constants. We notice that our solutions could be asymptotically de-Sitter, anti-de-Sitter or flat. We find the relevant quantities of the solutions, and discuss the properties of the solutions.

Figures

Figures reproduced from arXiv: 2501.07495 by the authors.

Figure 1
Figure 1. FIG. 1: The metric function [PITH_FULL_IMAGE:figures/full_fig_p007_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2: The behaviour of the cosmological constant in terms of (figure a) the spatial [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3: The behaviour of the dilaton field Φ( [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figures from the paper (11 more)
Figure 4
Figure 4. Figure 4: FIG. 4: The behaviour of the c-function with respect to the time coordinate in [PITH_FULL_IMAGE:figures/full_fig_p010_4.png]
Figure 5
Figure 5. Figure 5: FIG. 5: The electric fields (figure a) [PITH_FULL_IMAGE:figures/full_fig_p011_5.png]
Figure 6
Figure 6. Figure 6: FIG. 6: The metric function [PITH_FULL_IMAGE:figures/full_fig_p014_6.png]
Figure 7
Figure 7. Figure 7: figure 7. As we notice from figure 7a, the fluctuations in the dilaton field is not visible for [PITH_FULL_IMAGE:figures/full_fig_p014_7.png]
Figure 7
Figure 7. Figure 7: FIG. 7: The dilaton field Φ( [PITH_FULL_IMAGE:figures/full_fig_p015_7.png]
Figure 8
Figure 8. Figure 8: FIG. 8: The behaviour of the cosmological constant Λ in terms of (figure a): the number of [PITH_FULL_IMAGE:figures/full_fig_p015_8.png]
Figure 9
Figure 9. Figure 9: FIG. 9: The behaviour of the c-function for [PITH_FULL_IMAGE:figures/full_fig_p016_9.png]
Figure 10
Figure 10. Figure 10: FIG. 10: The electric fields (figure a): [PITH_FULL_IMAGE:figures/full_fig_p017_10.png]
Figure 11
Figure 11. Figure 11: FIG. 11: The metric function [PITH_FULL_IMAGE:figures/full_fig_p019_11.png]
Figure 12
Figure 12. Figure 12: FIG. 12 [PITH_FULL_IMAGE:figures/full_fig_p020_12.png]
Figure 13
Figure 13. Figure 13: FIG. 13: The electric fields (figure a): [PITH_FULL_IMAGE:figures/full_fig_p020_13.png]

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Works this paper leans on

57 extracted references · 55 canonical work pages

  1. [50]

    In figure 11, we show the behaviour of the metric function H(t, r, θ) in 5-dimensional spacetime (N = 4) for three different time slices

    for the five-dimensional Einstein-Maxwell-dilaton theory, based on the Bianchi type IX geometry. In figure 11, we show the behaviour of the metric function H(t, r, θ) in 5-dimensional spacetime (N = 4) for three different time slices. FIG. 11: The metric function H(t, r, θ) in (4 + 1)-dimensions, where the upper surface, middle surface and the lower surfa...

    work page

  2. [1]

    P. G. O. Freund, and M. A. Rubin, Phys. Lett.B97, 233 (1980)

    work page 1980

  3. [2]

    (68) We note that in equation (68), R′ is the p + 1-dimensional Ricci scalar, and Λ ′ = R′′/2, where R′′ is the q-dimensional Ricci scalar of the internal space

    + 2ΛDe−δϕ′ + 2Λ′e− 2 δ(p−1) ϕ′ ). (68) We note that in equation (68), R′ is the p + 1-dimensional Ricci scalar, and Λ ′ = R′′/2, where R′′ is the q-dimensional Ricci scalar of the internal space. We also note that in the action (68), δ and γ are the dilaton coupling constants, which are given by [47], δ = ( 2q (p − 1)(p + q − 1) )1/2, (69) γ = δ(2 − p). (...

    work page

  4. [3]

    Guica, T

    M. Guica, T. Hartman, W. Song and A. Strominger, Phys. Rev.D80, 124008 (2009)

    work page 2009

  5. [4]

    Kaluza, arXiv preprint arXiv:1803.08616

    Th. Kaluza, arXiv preprint arXiv:1803.08616

    arXiv

  6. [5]

    Gout´ eraux, J

    B. Gout´ eraux, J. Smolic, M. Smolic, K. Skenderis and M. Taylor, JHEP 1, 89 (2012)

    work page 2012

  7. [6]

    A. M. Ghezelbash, Phys. Rev.D91, 084003 (2015)

    work page 2015

  8. [7]

    M. M. Stetsko, The Europ. Phys. J.C79, 244 (2019)

    work page 2019

Show all 57 references
  1. [8]

    Mahapatra and P

    S. Mahapatra and P. Roy, Pratim, JHEP 11 138 (2018). 24

    2018

  2. [9]

    Goulart, arXiv preprint arXiv:1809.06533

    P. Goulart, arXiv preprint arXiv:1809.06533

    arXiv

  3. [10]

    Mahapatra, S

    S. Mahapatra, S. Priyadahshinee, G. Reddy and B. Shukla, Phys. Rev.D102, 024042 (2020)

    2020

  4. [11]

    Li, Phys

    L. Li, Phys. Lett.B767, 278 (2017)

    2017

  5. [12]

    Juli´ e,J

    F. Juli´ e,J. of Cosmo. and Astropar. Phys.10, 033 (2018)

    2018

  6. [13]

    Rougemont, J

    R. Rougemont, J. Grefa, M. Hippert, J. Noronha, J. Noronha-Hostler, I. Portillo and C. Ratti, Prog. in Par. and Nucl. Phys.135C, 104093 (2024)

    2024

  7. [14]

    Torii and T

    T. Torii and T. Shiromizu, Phys. Lett.B551, 161 (2003)

    2003

  8. [15]

    Heydari-Fard, M

    M. Heydari-Fard, M. Heydari-Fard and H. R. Sepangi, Phys. Rev.D105, 124009 (2022)

    2022

  9. [16]

    Bad ´ ıa and E

    J. Bad ´ ıa and E. F. Eiroa,Phys. Rev.D107, 124028 (2023)

    2023

  10. [17]

    Tan, Phys

    W. Tan, Phys. Rev.D102, 044054 (2020)

    2020

  11. [18]

    Tripathi, B

    A. Tripathi, B. Zhou, A. B. Abdikamalov, D. Ayzenberg and C. Bambi, JCAP 2107, 002 (2021)

    2021

  12. [20]

    H. L¨ u, P. Mao and J. Wu,JHEP 11 , 005 (2019)

    2019

  13. [21]

    Azreg-A ¨ ınou, A

    M. Azreg-A ¨ ınou, A. K. Ahmed and M. Jamil,Class. Quantum Grav.35 235001 (2018)

    2018

  14. [22]

    Li and H

    S. Li and H. Wei, Phys. Rev.D99, 064002 (2019)

    2019

  15. [23]

    Brito and C

    R. Brito and C. Pacilio, Phys. Rev.D98, 104042 (2018)

    2018

  16. [24]

    Khalil, N

    M. Khalil, N. Sennett, J. Steinhoff, J. Vines and A. Buonanno, Phys. Rev. D98, 104010 (2018)

    2018

  17. [25]

    Pacilio, Phys

    C. Pacilio, Phys. Rev.D98, 064055 (2018)

    2018

  18. [26]

    Azreg-A ¨ ınou, S

    M. Azreg-A ¨ ınou, S. Haroon, M. Jamil and M. Rizwan, Int. J. Mod. Phys. D28, 1950063 (2019)

    2019

  19. [27]

    J. F. Pedraza, W. Sybesma and M. R. Visser, Class. and Quant. Grav.36 054002, (2019)

    2019

  20. [28]

    Butler and A

    M. Butler and A. M. Ghezelbash, Int. J. of Mod. Phys.A34, 1950061 (2019)

    2019

  21. [29]

    Matsuno, H

    K. Matsuno, H. Ishihara and M. Kimura, Class. Quant. Grav.32 (2015) 215008

    2015

  22. [30]

    Ishihara, M

    H. Ishihara, M. Kimura and K. Matsuno, Phys. Rev.D93 (2016) 024037

    2016

  23. [31]

    D. Ida, H. Ishihara, M. Kimura, K. Matsuno, Y. Morisawa and S. Tomizawa, Class. Quant. Grav. 24 (2007) 3141. 25

    2007

  24. [32]

    Kanou, H

    Y. Kanou, H. Ishihara, M. Kimura, K. Matsun and T. Tatsuoka, Phys. Rev. D90 (2014) 084004

    2014

  25. [33]

    Kastor and J

    D. Kastor and J. H. Traschen, Phys. Rev.D47, 5370 (1993)

    1993

  26. [34]

    B. P. Abbott et al., Phys. Rev. Lett.116, 061102 (2016)

    2016

  27. [35]

    Ishihara, M

    H. Ishihara, M. Kimura and S. Tomizawa, Class. Quant. Grav.23, L89 (2006)

    2006

  28. [36]

    L. A. J. London, Nucl. Phys. B434, 709 (1995)

    1995

  29. [37]

    A. M. Ghezelbash, Phys. Rev.D78, 126002 (2008)

    2008

  30. [38]

    C. M. Yoo, H. Ishihara, M. Kimura, K. Matsuno and S. Tomizawa, Class. Quant. Grav.25, 095017 (2008)

    2008

  31. [39]

    Bali and S

    R. Bali and S. Dave, Pramana 56, 513 (2001)

    2001

  32. [40]

    K. R. Meyer, The American Mathematical Monthly108, 729 (2001)

    2001

  33. [41]

    Ashtekar and E

    A. Ashtekar and E. Wilson-Ewing, Edward, Phys. Rev.D80, 123532 (2009)

    2009

  34. [42]

    A. M. Ghezelbash, Phys. Rev.D74, 126004 (2006)

    2006

  35. [43]

    Maki and K

    T. Maki and K. Shiraishi, Class. and Quant. Grav.10, 2171 (1993)

    1993

  36. [44]

    A. A. Starobinsky, S.V. Sushkov and M. S. Volkov, Phys. Rev.D101, 064039 (2020)

    2020

  37. [45]

    Strominger, Andrew, JHEP 10, 034 (2001)

    A. Strominger, Andrew, JHEP 10, 034 (2001)

    2001

  38. [46]

    A. M. Ghezelbash, Phys. Rev.D81, 044027 (2010)

    2010

  39. [47]

    Gout´ eraux and E

    B. Gout´ eraux and E. Kiritsis,JHEP 12, 036 (2011)

    2011

  40. [48]

    Balasubramanian, J

    V. Balasubramanian, J. De Boer and D. Minic, Phys. Rev.D65, 123508 (2002)

    2002

  41. [49]

    Charmousis, D

    C. Charmousis, D. Langlois, D. Steer and R. Zegers, JHEP 0702 (2007) 064

    2007

  42. [51]

    Charmousis, B

    C. Charmousis, B. Gouteraux and J. Soda, Phys. Rev.D80 (2009) 024028

    2009

  43. [52]

    B. H. Fahim and A. M. Ghezelbash, The European Physical JournalC81, 1 (2021)

    2021

  44. [53]

    J. V. Rocha and M. Tomaˇ sevi´ c,Phys. Rev.D98, 104063 (2018)

    2018

  45. [54]

    A. M. Ghezelbash, Phys. Rev.D95, 064030 (2017)

    2017

  46. [55]

    Compere, K

    G. Compere, K. Murata and T. Nishioka, JHEP 09, 077 (2009)

    2009

  47. [56]

    A. M. Ghezelbash, JHEP 09, 045 (2009)

    2009

  48. [57]

    Castro, A

    A. Castro, A. Maloney and A. Strominger, Phys. Rev.D82, 024008 (2010)

    2010

  49. [58]

    A. M. Ghezelbash and H. Siahaan, Gen. Rel. and Grav.46, 1783 (2014). 26

    2014

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