REVIEW 3 major objections 4 minor 66 references
This paper establishes that for an effective non-commutative rotating black hole, the deformation shifts photon orbits and both ISCO branches inward, shrinks the shadow, and makes the geometric Hawking temperature and horizon angular veloci
Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →
T0 review · deepseek-v4-flash
2026-08-01 02:53 UTC pith:BJ4FOFDS
load-bearing objection The constrained fixed-Theta thermodynamics is the real new result; the geodesics are mostly Kerr-Newman substitutions, and the metric's physical status is unverified, so the paper deserves a serious referee but not acceptance as-is. the 3 major comments →
Constrained thermodynamics and geodesic observables of an effective non-commutative Kerr-like black hole
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
Core claim
On its own terms, the paper establishes that the metric ds^2 = -Delta/Sigma (dt - a sin^2 theta dphi)^2 + Sigma/Delta dr^2 + Sigma dtheta^2 + (sin^2 theta/Sigma)[a dt - (r^2+a^2) dphi]^2, with Sigma = r^2+a^2 cos^2 theta and Delta = r^2 - 2Mr + a^2 + beta_Theta, beta_Theta = 8M sqrt(Theta/pi), has a Kerr–Newman algebraic structure with a mass-dependent charge-like term. From this it derives an extremality bound Theta <= pi(M^2-a^2)^2/(64M^2), a zero-temperature remnant, stationary-limit surfaces and an ergoregion that thickens at the equator as Theta grows, and the equality Gamma_Theta dM = T_H dS + Omega_H dJ that defines the constrained first law, with exact conjugates tilde T = T_H/Gamma_
What carries the argument
The central object is the Boyer–Lindquist-like metric (13) with the single modified radial function Delta = r^2 - 2Mr + a^2 + beta_Theta, beta_Theta = 8M sqrt(Theta/pi) = M lambda_Theta. Retaining the Carter separability structure lets the entire Kerr–Newman geodesic toolkit—photon-region equations, shadow impact parameters, ISCO equation, frequency-shift formula—be adapted by replacing Q^2 with beta_Theta. The thermodynamic machinery rests on the identity beta_Theta = M lambda_Theta, which couples the deformation to mass, and on the factor Gamma_Theta = 1 - lambda_Theta r/[2(r^2+a^2)] that relates the geometric Hawking quantities to the reduced state-space conjugates.
Load-bearing premise
The load-bearing premise is that the truncated static lapse f(r) = 1 - 2M/r + 8M sqrt(Theta)/(sqrt(pi) r^2) can be rotated by the Newman–Janis algorithm into a metric that is a genuine black-hole solution of the parent field equations; the paper itself flags the algorithm as a prescription rather than a theorem and provides no field-equation verification, so if that rotation fails, every derived observable describes a toy geometry.
What would settle it
Substitute the rotating metric (13) into the complete Einstein–Kaluza–Klein field equations that the static seed is claimed to satisfy, and check whether they hold at order sqrt(Theta); if they do not, the horizon, thermodynamic, and geodesic results are properties of a metric that is not a solution of the underlying theory.
If this is right
- At fixed mass and spin, raising Theta lowers the extremal spin bound, shrinks the outer horizon, thickens the equatorial ergoregion, and leaves a zero-temperature remnant at extremality with M_rem = r_rem.
- The unstable photon rings and the shadow boundary move inward: the paper's equatorial-observer shadow plots shrink as Theta grows, and the static photon-sphere radius falls below 3M by 16 sqrt(Theta)/(3 sqrt(pi)).
- Every equatorial circular-orbit observable shifts: both prograde and retrograde ISCO radii decrease with Theta, so the inner edge of a geodesic accretion disk moves inward and the retrograde branch can fall below 6M.
- The fixed-Theta first law is not dM = T_H dS + Omega_H dJ; the geometric temperature and angular velocity must be rescaled by Gamma_Theta, and heat capacities computed from T_H alone misidentify the Davies-type critical points.
- A photon's observed redshift/blueshift requires the independent pair (s, sigma)—emitter orbit sign and tangential photon direction—so four distinct combinations exist; a prograde emitter can still deliver a blueshifted or redshifted photon depending on the photon branch.
Where Pith is reading between the lines
- Because beta_Theta mimics an electric charge in Kerr–Newman, shadow or continuum fits that allow a free 'charge' parameter could absorb the non-commutative effect; breaking the degeneracy would require combining shadow, ISCO, and thermal-spectrum measurements on the same object.
- The inward ISCO shift raises the gravitational binding energy of the innermost disk by a computable amount; computing the disk's radiative efficiency from the derived Es and Ls would turn the present orbital formulas into a direct observational prediction.
- The extreme-regime results—remnant mass, zero-temperature endpoint, and near-extremal photon rings—sit outside the controlled domain of the truncated seed (which omits O(M Theta^{3/2}/r^4) terms), so they are indications of a toy model unless a full non-commutative solution reproduces them.
- The Gamma_Theta rescaling between geometric and conjugate thermodynamics is a generic template: any effective metric whose charge-like parameter is a function of M, not an independent variable, will display a similar split between Hawking quantities and first-law conjugates.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The paper constructs an effective rotating metric by applying the Newman-Janis algorithm to the truncated non-commutative Schwarzschild lapse f(r)=1-2M/r+8M sqrt(Theta)/(sqrt(pi) r^2) (Eq. (1)). The resulting Boyer-Lindquist metric (13)-(14) is of Kerr-Newman form with beta_Theta = 8M sqrt(Theta)/sqrt(pi). The authors derive the horizon structure and extremality bound, a constrained fixed-Theta thermodynamics in which the fundamental relation M(S,J,Theta) replaces the naive dM=T_H dS+Omega_H dJ with conjugate quantities tilde T and tilde Omega, several heat capacities, the spherical photon region, equatorial light rings, shadow boundary, prograde/retrograde ISCO equations, and two-sign frequency shifts. The headline physical claims are that increasing Theta shifts photon orbits inward, reduces the shadow, and moves both ISCO branches inward, while the geometric Hawking temperature differs from the constrained thermodynamic conjugate.
Significance. If accepted as an exact property of the stated ansatz, the paper's algebra is sound: I checked the horizon roots (22), temperature (28), light-ring equation (111), photon-region impact parameters (106)-(107), and static ISCO expansion (131)-(132); they are internally consistent and reduce to Kerr when Theta=0. A clear strength is that the observables are derived, not fitted, and the fixed-Theta thermodynamic conjugates follow from a closed-form fundamental relation. The distinction between geometric Hawking quantities and constrained conjugates (Eqs. (54)-(60)) is conceptually useful. The main limitation is that the physical status of the rotating metric as a 'non-commutative black hole' depends on an unverified NJA rotation of a truncated seed, so the significance of the observable predictions is conditional on accepting this effective metric as physically meaningful.
major comments (3)
- [Sec. II.A (Eqs. (12)-(14))] The NJA rotation of seed (1) is never checked against field equations. The paper itself states in Sec. II.A that the generated metric is 'a candidate rotating geometry until... verified explicitly,' but no such verification is supplied. Since beta_Theta = 8M sqrt(Theta)/sqrt(pi) is mass-dependent and is not sourced by any explicit field, the rotating metric is not shown to be a non-commutative black hole solution. The abstract's observable claims ('non-commutative correction...') are therefore properties of an ansatz, not established physical predictions. Please either identify a parent action/matter source whose equations admit (13) or reframe the title/abstract/conclusions to describe a Kerr-Newman-like toy model.
- [Sec. II.E; Sec. III.B-C; Sec. V.C] The seed (1) is derived in the regime r >> sqrt(Theta), but central extremal results — remnant (30)-(31), the static ISCO endpoint q=1 with x=4, and the strong-deformation crossing of the retrograde ISCO below 6M — are evaluated near r ~ sqrt(Theta). There the neglected O(M Theta^{3/2}/r^4) term in (1) has the same scaling as the retained beta term (both ~ M/sqrt(Theta)), so the small-Theta expansion does not control those regimes. The caveat in Sec. II does not protect quantitative claims. Please use the full mass function or explicitly mark extreme-regime results as illustrative and outside the controlled domain.
- [Sec. VI.B-C (Eq. (150), Fig. 5)] The frequency-shift section stops at the local emission formula. The text mentions that a photon must satisfy the global escape condition, but Eq. (150) and Fig. 5 do not implement it. For some (s,sigma) combinations at small r_e the tangential photon may be captured before reaching a distant static observer, so z_{sigma;s} as plotted is not necessarily a distant-observer observable. Please either impose the photon-region/escape criterion or state clearly that the plotted quantity is a local emission redshift for a hypothetically asymptotic observer.
minor comments (4)
- [Sec. III.A, III.C] There are duplicated sentences: in Sec. III.A 'Thus, T_H and Omega_H remain the geometric horizon quantities, Thus, T_H...' and in Sec. III.C 'At such a point C diverges and changes sign, At this point...'. Eq. (72) also contains a repeated 'eC_J,Theta = eC_J,Theta ='. Please clean up these textual glitches.
- [Eq. (143)] The convention for the photon-direction sign sigma is stated after Eq. (143), but a reader can initially confuse it with the emitter-orbit sign s introduced in Eq. (121). Consider defining both signs explicitly in a single sentence before Eq. (143).
- [Fig. 5] Only the prograde emitter (s=+1) is plotted. Since the paper emphasizes the independence of s and sigma, showing all four (s,sigma) combinations, or at least stating that the other cases are analogous, would make the claim complete.
- [References] Reference [41] is formatted inconsistently with the surrounding entries ('Araujo Filho, A. A., et al.'). Please convert to the journal's citation style.
Circularity Check
No circularity: all observable results are exact consequences of an explicitly stated metric ansatz, with no fitted parameters and no load-bearing self-citation.
full rationale
The paper is self-contained in its derivation chain. Sections II–VI start from the explicit rotating metric ansatz in Eqs. (13)–(14), with Δ = r² − 2Mr + a² + βΘ and βΘ = 8M√Θ/√π, and then compute horizons, surface gravity, constrained first law, photon region, shadow, ISCO, and frequency shifts as exact algebraic and geodesic consequences of that ansatz. No quantity entering the shadow or ISCO is fitted; the deformation parameter is fixed by the seed lapse (1) before any observable is computed, and the Kerr limit is recovered when Θ = 0 as an external check. The constrained thermodynamics follows from the closed-form fundamental relation (56), so the conjugates in Eqs. (58)–(59) are exact partial derivatives of M(S,J,Θ) and are not defined in terms of the geometric quantities they are compared with. The Newman–Janis procedure is standard, and the paper explicitly flags in Section II.A that the generated metric is a candidate rotating geometry pending field-equation verification; this is an unverified physical premise, not a circular reduction. Self-citations to earlier shadow/NJA papers are not load-bearing because the relevant geodesic equations and photon-region formulas are re-derived in the text and the procedure is also anchored in external references. No circular step is present.
Axiom & Free-Parameter Ledger
free parameters (1)
- Theta (non-commutative deformation parameter)
axioms (4)
- ad hoc to paper The truncated lapse f(r) = 1 - 2M/r + 8M sqrt(Theta)/(sqrt(pi) r^2) is adopted as the defining seed metric (Eq. (1)).
- domain assumption The Newman–Janis algorithm produces the correct rotating geometry for this seed.
- domain assumption Entropy is given by the Bekenstein–Hawking area law S = A/4.
- standard math The standard Carter-separability and geodesic formalism (surface gravity, photon region, ISCO) applies to the effective metric.
invented entities (1)
-
Mass-dependent charge-like deformation beta_Theta = 8M sqrt(Theta)/sqrt(pi)
no independent evidence
read the original abstract
We investigate the horizon structure, constrained thermodynamics, and geodesic properties of an effective Kerr-like black hole in a non-commutative background. Deformation modifies the radial geometry through a mass-dependent charge-like contribution, while preserving the separability of the geodesic equations. We determine the conditions for horizon existence, identify the extremal zero-temperature configuration, and analyze the stationary-limit surfaces and the ergoregion. Special attention is paid to the thermodynamic interpretation of the model, where the geometric Hawking quantities are distinguished from the conjugate variables associated with the constrained state space at fixed non-commutative deformation parameter. The canonical and grand-canonical heat capacities are derived to characterize their ensemble-dependent local thermal behavior. We also obtain the spherical photon region, equatorial light rings, and shadow boundary, showing that the deformation shifts the characteristic photon orbits inwards and reduces the overall size of the shadow. Timelike circular motion is studied through the innermost stable circular orbit, where non-commutative correction produces an inward shift of both the prograde and retrograde branches. Finally, invariant photon frequency shifts are obtained by treating the emitter's orbital direction and the photon's tangential emission direction as independent physical choices.
Figures
Reference graph
Works this paper leans on
-
[1]
fixeda”, “fixedJ
Horizon entropy and its dependence on the deformation parameter Throughout this section, we assume that the gravitational sector is described by the Einstein–Hilbert action and that the non-commutative correction is encoded in an effective matter source. Under this assumption, the horizon entropy obeys the Bekenstein–Hawking area law. Atr=r +, the nonvani...
2025
-
[2]
String theory and noncommutative geometry,
N. Seiberg and E. Witten, “String theory and noncommutative geometry,” JHEP09(1999) 032
1999
-
[3]
Quantum field theory on noncommutative spaces,
R. J. Szabo, “Quantum field theory on noncommutative spaces,” Phys. Rept.378(2003) 207–299
2003
-
[4]
Noncommutative field theory,
M. R. Douglas and N. A. Nekrasov, “Noncommutative field theory,” Rev. Mod. Phys.73(2001) 977–1029
2001
-
[5]
Noncommutative black holes, the final appeal to quantum gravity: a review,
P. Nicolini, “Noncommutative black holes, the final appeal to quantum gravity: a review,” Int. J. Mod. Phys. A24(2009) 1229–1308
2009
-
[6]
Feynman path integral on the noncommutative plane,
A. Smailagic and E. Spallucci, “Feynman path integral on the noncommutative plane,” J. Phys. A36(2003) L467–L471
2003
-
[7]
Thermodynamics and evaporation of the noncommutative black hole,
Y . S. Myung, Y .-W. Kim, and Y .-J. Park, “Thermodynamics and evaporation of the noncommutative black hole,” JHEP02(2007) 012
2007
-
[8]
Charged rotating noncommutative black holes,
L. Modesto and P. Nicolini, “Charged rotating noncommutative black holes,” Phys. Rev. D82(2010) 104035
2010
-
[9]
Noncommutative black hole thermodynamics,
R. Banerjee, B.R. Majhi, and S. Samanta, “Noncommutative black hole thermodynamics,” Physical Review D—Particles, Fields, Gravi- tation, and Cosmology, 77(12) (2008) 124035
2008
- [10]
-
[11]
Thermodynamics of a Bardeen black hole in noncommutative space,
M. Sharif and W. Javed, “Thermodynamics of a Bardeen black hole in noncommutative space,” Canadian Journal of Physics, 89(10) (2011) 1027-1033
2011
-
[12]
Non-commutativity in Hayward spacetime,
N. Heidari, A.A. Ara ´ujo Filho and I.P. Lobo, “Non-commutativity in Hayward spacetime,” JCAP,09(2025) 051. 20
2025
-
[13]
A non-commutative Kalb-Ramond black hole,
A.A. Ara ´ujo Filho, N. Heidari, and I.P. Lobo, “A non-commutative Kalb-Ramond black hole,” JCAP,09(2025) 076
2025
-
[14]
Quasinormal modes in noncommutative Schwarzschild black holes,
Y . Zhao, Y . Cai, S. Das, G. Lambiase, E.N. Saridakis and E.C. Vagenas, “Quasinormal modes in noncommutative Schwarzschild black holes,” Nuclear Physics B, 1004 (2024) 116545
2024
-
[15]
Absorption, scattering and shadow by a noncommutative black hole with global monopole,
M.A. Anacleto, F.A. Brito, J.A.V . Campos and E. Passos, “Absorption, scattering and shadow by a noncommutative black hole with global monopole,” Eur. Phys. J. C, 83(4) (2023) 298
2023
-
[16]
Absorption and scattering of a noncommutative black hole,
M.A. Anacleto, F.A. Brito, J.A.V . Campos and E. Passos, “Absorption and scattering of a noncommutative black hole,” Phys. Lett. B803, 135334 (2020)
2020
-
[17]
Exploring non-commutativity as a perturbation in the Schwarzschild black hole: quasinormal modes, scattering, and shadows,
N. Heidari, H. Hassanabadi, A.A. Ara ´ujo Filho and J. Kriz, “Exploring non-commutativity as a perturbation in the Schwarzschild black hole: quasinormal modes, scattering, and shadows,” Eur. Phys. J. C, 84(6) (2024) 566
2024
-
[18]
Corrections to Schwarzschild solution in noncommutative gauge theory of gravity,
M. Chaichian, A. Tureanu and G. Zet, “Corrections to Schwarzschild solution in noncommutative gauge theory of gravity,” Phys. Lett. B 660, 573–578 (2008)
2008
-
[19]
Gravitational field of a spinning mass as an example of algebraically special metrics,
R. P. Kerr, “Gravitational field of a spinning mass as an example of algebraically special metrics,” Phys. Rev. Lett.11(1963) 237–238
1963
-
[20]
Global structure of the Kerr family of gravitational fields,
B. Carter, “Global structure of the Kerr family of gravitational fields,” Phys. Rev.174(1968) 1559–1571
1968
-
[21]
Chandrasekhar,The Mathematical Theory of Black Holes, Oxford University Press, Oxford (1983)
S. Chandrasekhar,The Mathematical Theory of Black Holes, Oxford University Press, Oxford (1983)
1983
-
[22]
Timelike and null geodesics in the Kerr metric,
J. M. Bardeen, “Timelike and null geodesics in the Kerr metric,” inBlack Holes, eds. C. DeWitt and B. S. DeWitt, Gordon and Breach, New York (1973), pp. 215–239
1973
-
[23]
Spherical photon orbits around a Kerr black hole,
E. Teo, “Spherical photon orbits around a Kerr black hole,” Gen. Rel. Grav.35(2003) 1909–1926
2003
-
[24]
Rotating black holes: Locally nonrotating frames, energy extraction, and scalar synchrotron radiation,
J. M. Bardeen, W. H. Press, and S. A. Teukolsky, “Rotating black holes: Locally nonrotating frames, energy extraction, and scalar synchrotron radiation,” Astrophys. J.178, 347–370 (1972)
1972
-
[25]
Equatorial circular motion in Kerr spacetime,
D. Pugliese, H. Quevedo, and R. Ruffini, “Equatorial circular motion in Kerr spacetime,” Phys. Rev. D84, 044030 (2011)
2011
-
[26]
Astrophysics of black holes,
I. D. Novikov and K. S. Thorne, “Astrophysics of black holes,” inBlack Holes (Les Astres Occlus), edited by C. DeWitt and B. S. DeWitt (Gordon and Breach, New York, 1973), pp. 343–450
1973
-
[27]
Disk-accretion onto a black hole. I. Time-averaged structure of accretion disk,
D. N. Page and K. S. Thorne, “Disk-accretion onto a black hole. I. Time-averaged structure of accretion disk,” Astrophys. J.191, 499–506 (1974)
1974
-
[28]
Disk-accretion onto a black hole. II. Evolution of the hole,
K. S. Thorne, “Disk-accretion onto a black hole. II. Evolution of the hole,” Astrophys. J.191, 507–520 (1974)
1974
-
[29]
The effects of redshifts and focusing on the spectrum of an accretion disk around a Kerr black hole,
C. T. Cunningham, “The effects of redshifts and focusing on the spectrum of an accretion disk around a Kerr black hole,” Astrophys. J. 202, 788–802 (1975)
1975
-
[30]
Equatorial circular orbits in the Kerr–de Sitter spacetimes,
Z. Stuchl ´ık and P. Slan´y, “Equatorial circular orbits in the Kerr–de Sitter spacetimes,” Phys. Rev. D69, 064001 (2004)
2004
-
[31]
A metric for rapidly spinning black holes suitable for strong-field tests of the no-hair theorem,
T. Johannsen and D. Psaltis, “A metric for rapidly spinning black holes suitable for strong-field tests of the no-hair theorem,” Phys. Rev. D83, 124015 (2011)
2011
-
[32]
Testing black hole candidates with electromagnetic radiation,
C. Bambi, “Testing black hole candidates with electromagnetic radiation,” Rev. Mod. Phys.89, 025001 (2017)
2017
-
[33]
Circular geodesics of Bardeen and Ay ´on-Beato–Garc´ıa regular black-hole and no-horizon spacetimes,
Z. Stuchl ´ık and J. Schee, “Circular geodesics of Bardeen and Ay ´on-Beato–Garc´ıa regular black-hole and no-horizon spacetimes,” Int. J. Mod. Phys. D24, 1550020 (2015)
2015
-
[34]
Noncommutative geometry inspired Schwarzschild black hole,
P. Nicolini, A. Smailagic, and E. Spallucci, “Noncommutative geometry inspired Schwarzschild black hole,” Phys. Lett. B632, 547–551 (2006)
2006
-
[35]
Noncommutative geometry inspired charged black holes,
S. Ansoldi, P. Nicolini, A. Smailagic, and E. Spallucci, “Noncommutative geometry inspired charged black holes,” Phys. Lett. B645, 261–266 (2007)
2007
-
[36]
Noncommutative geometry inspired dirty black holes,
P. Nicolini and E. Spallucci, “Noncommutative geometry inspired dirty black holes,” Class. Quantum Grav.27, 015010 (2010)
2010
-
[37]
‘Kerrr’ black hole: The Lord of the String,
A. Smailagic and E. Spallucci, “‘Kerrr’ black hole: The Lord of the String,” Phys. Lett. B688, 82–87 (2010)
2010
-
[38]
Charged rotating noncommutative black holes,
L. Modesto and P. Nicolini, “Charged rotating noncommutative black holes,” Phys. Rev. D82, 104035 (2010)
2010
-
[39]
Shadow of noncommutative geometry inspired black hole,
S.-W. Wei, P. Cheng, Y . Zhong, and X.-N. Zhou, “Shadow of noncommutative geometry inspired black hole,” JCAP08, 004 (2015)
2015
-
[40]
Accretion onto a noncommutative geometry inspired black hole,
R. Kumar and S. G. Ghosh, “Accretion onto a noncommutative geometry inspired black hole,” Eur. Phys. J. C77, 577 (2017)
2017
-
[41]
Absorption and scattering of a noncommutative black hole,
M. A. Anacleto, F. A. Brito, J. A. V . Campos, and E. Passos, “Absorption and scattering of a noncommutative black hole,” Phys. Lett. B 803(2020) 135334
2020
-
[42]
A., et al
Ara ´ujo Filho, A. A., et al. ”Effects of non-commutative geometry on black hole properties.” Physics of the Dark Universe 46 (2024): 101630
2024
-
[43]
S Capozziello, S Zare, DF Mota, and H Hassanabadi, JCAP 05 (2023) 027
2023
-
[44]
Capozziello, S
S. Capozziello, S. Zare, L. M. Nieto, and H. Hassanabadi, Phys. Dark Universe 50 (2025) 102065
2025
-
[45]
Note on the Kerr spinning-particle metric,
E. T. Newman and A. I. Janis, “Note on the Kerr spinning-particle metric,” J. Math. Phys.6, 915–917 (1965). doi:10.1063/1.1704350
-
[46]
Metric of a rotating, charged mass,
E. T. Newman, E. Couch, K. Chinnapared, A. Exton, A. Prakash, and R. Torrence, “Metric of a rotating, charged mass,” J. Math. Phys. 6, 918–919 (1965). doi:10.1063/1.1704351
-
[47]
Uniqueness of the Newman–Janis algorithm in generating the Kerr–Newman metric,
S. P. Drake and P. Szekeres, “Uniqueness of the Newman–Janis algorithm in generating the Kerr–Newman metric,” Gen. Relativ. Gravit. 32, 445–458 (2000). doi:10.1023/A:1001920232180
-
[48]
C. Bambi and L. Modesto, “Rotating regular black holes,” Phys. Lett. B721, 329–334 (2013). doi:10.1016/j.physletb.2013.03.025
-
[49]
Generating rotating regular black hole solutions without complexification,
M. Azreg-A ¨ınou, “Generating rotating regular black hole solutions without complexification,” Phys. Rev. D90, 064041 (2014). doi:10.1103/PhysRevD.90.064041
-
[50]
M. Azreg-A¨ınou, “From static to rotating to conformal static solutions: Rotating imperfect fluid wormholes with(out) electric or magnetic field,” Eur. Phys. J. C74, 2865 (2014). doi:10.1140/epjc/s10052-014-2865-8
-
[51]
Janis–Newman algorithm: Generating rotating and NUT charged black holes,
H. Erbin, “Janis–Newman algorithm: Generating rotating and NUT charged black holes,” Universe3, 19 (2017). doi:10.3390/universe3010019
-
[52]
Black hole shadow in a general rotating spacetime obtained through the Newman–Janis algorithm,
R. Shaikh, “Black hole shadow in a general rotating spacetime obtained through the Newman–Janis algorithm,” Phys. Rev. D100, 024028 (2019). doi:10.1103/PhysRevD.100.024028
-
[53]
H. C. D. Lima Junior, L. C. B. Crispino, P. V . P. Cunha, and C. A. R. Herdeiro, “Spinning black holes with a separable Hamilton–Jacobi equation from a modified Newman–Janis algorithm,” Eur. Phys. J. C80, 1036 (2020). doi:10.1140/epjc/s10052-020-08572-w. 21
-
[54]
Applicability of the Newman–Janis algorithm to black hole solutions of modified gravity theories,
D. Hansen and N. Yunes, “Applicability of the Newman–Janis algorithm to black hole solutions of modified gravity theories,” Phys. Rev. D88, 104020 (2013). doi:10.1103/PhysRevD.88.104020
-
[55]
Calculating black hole shadows: review of analytical studies,
V . Perlick, and O. Y . Tsupko, “Calculating black hole shadows: review of analytical studies,” Phys. Rept.947(2022) 1–39
2022
-
[56]
S. Zare, L. M. Nieto, F. Hosseinifar, X.-H. Feng, and H. Hassanabadi, Phys. Lett. B 859 (2024) 139125
2024
-
[57]
S. Zare, L. M. Nieto, X.-H. Feng, S.-H. Dong, and H. Hassanabadi, JCAP 08 (2024) 041
2024
-
[58]
S. Zare, T. Zhu, L. M. Nieto, S. Lu, and H. Hassanabadi, JCAP 01 (2026) 059
2026
-
[59]
S. Zare, F. Hosseinifar, L. M. Nieto, D. J. Gogoi, K. Boshkayev, A. Urazalina, and H. Hassanabadi, Eur. Phys. J. C 86 (2026) 160
2026
-
[60]
H. Hassanabadi, A. Guvendi, F. Kafikang, T. Sathiyaraj, and S. Zare, arXiv:2512.18512
-
[61]
F. Hosseinifar, S. Mamedov, K. Boshkayev, S. Zare, F. Studniˇcka, and H. Hassanabadi, arXiv:2605.20239
-
[62]
H. Hassanabadi, M. R. R. Good, S. Zare, O. Luongo and F. Kafikang, arXiv:2607.11979
-
[63]
Kerr black hole parameters in terms of the redshift/blueshift of photons emitted by geodesic particles,
A. Herrera-Aguilar and U. Nucamendi, “Kerr black hole parameters in terms of the redshift/blueshift of photons emitted by geodesic particles,” Phys. Rev. D92(2015) 045024
2015
-
[64]
Thermodynamics of black holes,
P. C. W. Davies, “Thermodynamics of black holes,” Rept. Prog. Phys.41(1978) 1313–1355
1978
-
[65]
Noncommutative black hole thermodynamics,
R. Banerjee, B. R. Majhi, and S. Samanta, “Noncommutative black hole thermodynamics,” Phys. Rev. D77(2008) 124035
2008
-
[66]
Towards noncommutative quantum black holes,
J. C. L ´opez-Dom´ınguez, O. Obreg ´on, M. Sabido, and C. Ram ´ırez, “Towards noncommutative quantum black holes,” Phys. Rev. D74 (2006) 084024
2006
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.