{"total":26,"items":[{"citing_arxiv_id":"2605.23047","ref_index":52,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On Thermodynamics of Charged Black Holes, Swampland, and Dark Matter","primary_cat":"hep-th","submitted_at":"2026-05-21T21:26:52+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18371","ref_index":80,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dyonic Black Holes in Lorentz-Violating Gravity with a Background Kalb--Ramond Field","primary_cat":"gr-qc","submitted_at":"2026-05-18T13:20:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"An exact dyonic black hole metric is derived in Lorentz-violating gravity with background Kalb-Ramond field and nonminimal EM coupling; geodesics and extended thermodynamics are analyzed showing parameter-dependent shadows and first-order phase transitions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16536","ref_index":23,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Quantum-statistical constraints on Kerr-anti-de Sitter thermodynamics","primary_cat":"gr-qc","submitted_at":"2026-05-15T18:32:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Quantum-statistical constraints restrict the infinite family of KadS thermodynamic descriptions to a subclass that reduces to Schwarzschild-AdS and Kerr cases in appropriate limits, with uniqueness for co-rotating and volume-coincident descriptions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15655","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Critical slowing down of black hole phase transition and universal dynamic scaling in AdS black holes","primary_cat":"hep-th","submitted_at":"2026-05-15T06:24:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Black hole phase transitions in AdS spacetime show critical slowing down with relaxation time scaling as τ = |ε|^{-2/3}, and this exponent is the same for RN-AdS, Kerr-AdS, and Bardeen black holes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12632","ref_index":71,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Criticality Quenching and Microstructure of Quintessence-AdS Black Holes","primary_cat":"hep-th","submitted_at":"2026-05-12T18:13:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Quintessence in RN-AdS black holes makes repulsive interactions dominate at high electric potentials while keeping interaction strength roughly constant across the phase transition.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Azreg-A¨ ınou, Phys. Rev. D90, no.6, 064041 (2014) doi:10.1103/PhysRevD.90.064041 [arXiv:1405.2569 [gr-qc]]. [69] E. Ayon-Beato and A. Garcia, Phys. Rev. Lett.80, 5056-5059 (1998) doi:10.1103/PhysRevLett.80.5056 [arXiv:gr-qc/9911046 [gr-qc]]. [70] G. Q. Li, Phys. Lett. B735, 256-260 (2014) doi:10.1016/j.physletb.2014.06.047 [arXiv:1407.0011 [gr- qc]]. [71] D. Kubiznak and R. B. Mann, \"P-V criticality of charged AdS black holes\", J. High Energy Phys. 07 (2012) 033 [arXiv:1205.0559 [hep-th]]. [72] R.-G. Cai, Li-Ming Cao, Li Li, Run-Qiu Yang, \"P-V criticality in the extended phase space of Gauss- Bonnet black holes in AdS space\", J. High Energy Phys. 09 (2013) 005 [arXiv:1306.6233 [gr-qc]]. [73] B. R. Majhi and S."},{"citing_arxiv_id":"2605.02429","ref_index":146,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Black Hole Thermodynamics via Tsallis Statistical Mechanics and Phase Transitions Probed by Optical Characteristics","primary_cat":"gr-qc","submitted_at":"2026-05-04T10:27:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Tsallis statistics applied to Reissner-Nordström black holes yields a generalized entropy leading to Van der Waals-like phase transitions whose critical behavior is reflected in photon-sphere observables.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"B. Mann, and D. Kubiznak, Extended phase space thermodynamics for charged and rotating black holes and Born-Infeld vacuum polarization, JHEP11, 110, arXiv:1208.6251 [hep-th]. [153] M. B. J. Poshteh, B. Mirza, and Z. Sherkatghanad, Phase transition, critical behavior, and critical exponents of myers-perry black holes, Phys. Rev. D88, 024005 (2013). [154] M. E. Fisher, The theory of critical point singularities, inCritical Phenomena, edited by M. S. Green (Academic Press, 1971) pp. 1-99. [155] H. E. Stanley,Introduction to Phase Transitions and Critical Phenomena(Oxford University Press, Oxford, UK, 1971). [156] N. Goldenfeld,Lectures on Phase Transitions and the Renormalization Group(Addison- Wesley, Reading, MA, 1992)."},{"citing_arxiv_id":"2605.01934","ref_index":28,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Scalar-Electromagnetic Couplings as Source of Deformed Black Hole: From Shadows to Thermodynamic Topology","primary_cat":"gr-qc","submitted_at":"2026-05-03T15:31:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A scalar-NED coupled black hole metric is reconstructed from an effective geometry, yielding EHT bounds on magnetic charge, Hawking-Page transition, and topological equivalence to the Reissner-Nordström solution.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Davies, \"Thermodynamics of Black Holes,\" Proc. Roy. Soc. Lond. A353(1977), 499-521 [26] D. Kastor, S. Ray and J. Traschen, \"Enthalpy and the Mechanics of AdS Black Holes,\" Class. Quant. Grav.26 (2009), 195011 [arXiv:0904.2765 [hep-th]]. [27] B. P. Dolan, \"Pressure and volume in the first law of black hole thermodynamics,\" Class. Quant. Grav.28 (2011), 235017 [arXiv:1106.6260 [gr-qc]]. [28] D. Kubiznak and R. B. Mann, \"P-V criticality of charged AdS black holes,\" JHEP07(2012), 033 [arXiv:1205.0559 [hep-th]]. [29] S. W. Hawking and D. N. Page, \"Thermodynamics of Black Holes in anti-De Sitter Space,\" Commun. Math. Phys.87(1983), 577 [30] E. Witten, \"Anti-de Sitter space, thermal phase transi- tion, and confinement in gauge theories,\" Adv."},{"citing_arxiv_id":"2604.27449","ref_index":43,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Phase-Space Contractions of Carrollian Black-Hole Thermodynamics","primary_cat":"hep-th","submitted_at":"2026-04-30T05:44:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Carrollian contraction of Schwarzschild-AdS thermodynamics requires rescaling the time generator and G such that the extended first law remains finite, yielding T to 0 and S to infinity with finite T delta S and V delta P.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.00037","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Topology of black hole thermodynamics: A brief review","primary_cat":"gr-qc","submitted_at":"2026-04-28T09:28:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Topological numbers categorize black hole systems into universality classes based on thermodynamic behavior, with calculations for critical points and phase transitions.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Subsequently, employ- ing the Maxwell equal area law on the isothermal curve or observing the swallowtail behavior of the Gibbs free energy facilitates the determination of first-order small- large black hole phase transitions. Generally, the coexis- tence curve ends at a critical point, indicating a second- order phase transition, which can be resolved by [13] (∂V P) = (∂ V,V P) = 0.(32) Alternatively, from the differential form of the Gibbs free energydG=−SdT+V dP+ P i Yidxi, the critical point can also be determined by [39] (∂ST) = (∂ S,ST) = 0.(33) To delineate the topology concerning the critical point, we will consider the latter scenario. As depicted in Eq. (31), the temperature can be represented as a function"},{"citing_arxiv_id":"2604.13104","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Nonequilibrium crossover in the supercritical region from quench dynamics","primary_cat":"cond-mat.stat-mech","submitted_at":"2026-04-10T15:42:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Quench dynamics in a holographic superfluid reveal a nonequilibrium crossover line in the supercritical region defined by a turning point in invasion velocity.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"2101, 013105 (2021), arXiv:2006.01156 [cond-mat.quant- gas]. [3] J. L. Jim' enez, S. P. G. Crone, E. Fogh, M. E. Za- yed, R. Lortz, E. Pomjakushina, K. Conder, A. M. L¨ auchli, L. Weber, S. Wessel, A. Honecker, B. Normand, C. R¨ uegg, P. Corboz, H. M. Rønnow, and F. Mila, Na- ture592, 370-375 (2021). [4] V. V. Brazhkin and K. Trachenko, Physics Today65, 68 (2012). [5] D. Kubiznak and R. B. Mann, JHEP07, 033 (2012), arXiv:1205.0559 [hep-th]. [6] D. Kubiznak, R. B. Mann, and M. Teo, Class. Quant. Grav.34, 063001 (2017), arXiv:1608.06147 [hep-th]. [7] R.-G. Cai, L.-M. Cao, L. Li, and R.-Q. Yang, JHEP09, 005 (2013), arXiv:1306.6233 [gr-qc]. [8] S.-W. Wei and Y.-X. Liu, Phys. Rev. D90, 044057 (2014), arXiv:1402.2837 [hep-th]."},{"citing_arxiv_id":"2604.08629","ref_index":7,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Thermodynamics and phase transitions of $\\kappa$-deformed Schwarzschild-AdS black holes","primary_cat":"gr-qc","submitted_at":"2026-04-09T16:22:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"κ-deformation induces critical behavior and phase transitions in uncharged Schwarzschild-AdS black holes with Pc vc/Tc ≈ 0.37 independent of κ and a double-loop G-T structure.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ume, while incorporating conserved charges such as elec- tric charge and angular momentum. In this framework, the BH mass is interpreted as enthalpy rather than in- ternal energy [5, 6]. In this regard, charged AdS BHs have been shown to exhibitP-Vcriticality, with critical behaviour analogous to the Van der Waals phase tran- sition in ordinary liquid-gas systems [7]. Subsequently, critical behaviour and phase transitions of various AdS ∗ nathith@irb.hr † vishnu@hunnu.edu.cn ‡ pxwu@hunnu.edu.cn BHs in the extended phase space have been extensively investigated [8-20]. Although Einstein gravity provides a robust descrip- tion of gravitational phenomena, it is expected to break down in the strong-gravity regime, where quantum fluc-"},{"citing_arxiv_id":"2604.08315","ref_index":1,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Unifying topological, geometric, and complex classifications of black hole thermodynamics","primary_cat":"gr-qc","submitted_at":"2026-04-09T14:48:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Three classification schemes for black hole thermodynamics are equivalent, with the count of temperature extrema determining the class in each framework.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the geometric properties of black holes, which are exact spacetime solutions predicted by general relativity, has long held a central position in gravitational theory re- search. In recent years, with the development of black hole thermodynamics, particularly the discovery of first- order phase transitions analogous to those of van der Waals fluids [1], attention has turned to whether these thermodynamic phenomena are fundamentally connected to the geometric properties of black holes. Recent studies have revealed profound intrinsic connec- tions between the thermodynamic, geometric, and topo- logical properties of black holes. Investigations into the local geometric properties of the black hole temperature"},{"citing_arxiv_id":"2604.08170","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Thermodynamics and orbital structure of anti-de Sitter black holes in Palatini-inspired nonlinear electrodynamics","primary_cat":"gr-qc","submitted_at":"2026-04-09T12:28:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"An exact AdS extension of the PINLED black hole is derived from the Einstein-Hilbert action plus nonlinear EM sector, preserving the original parametric form while adding the standard AdS lapse term, followed by full thermodynamic and geodesic analysis.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"often called black-hole chemistry [26], has since been ap- plied to a broad spectrum of solutions, uncovering phe- nomena such as reentrant phase transitions [27], triple points [28], and superfluid-like transitions [29] that have no counterpart in the asymptotically flat setting. In the NLE sector, extended phase-space thermodynamics has been investigated for Born-Infeld AdS black holes [30], for exponential NLE [10], and for a variety of other mod- els [31, 32], consistently revealing that the nonlinear cou- pling deforms the critical point and modifies the phase- transition structure relative to the RN-AdS baseline. Independently of their thermodynamic properties, black-hole geometries are characterized by their geodesic structure. The unstable circular photon orbit, the"},{"citing_arxiv_id":"2604.05785","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probabilistic Evolution of Black Hole Thermodynamic States via Fokker-Planck Equation","primary_cat":"gr-qc","submitted_at":"2026-04-07T12:21:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Solving the Fokker-Planck equation shows RN-AdS black hole phase transitions synchronize with a peak in entropy production rate, driven by maximum thermodynamic dissipation.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"namics has been rigorously refined. Wald defined black hole thermodynamic varibles as the Noether charge [1], providing a geometric foundation applicable to general grav- ity theories [2-5]. The interpretation of the cosmological constant as pressure [6-8] leads to the extended phase space formalism, which reveals that AdS black holes ex- hibit Van der Waals-like phase structures [9]. More recently, motivated by the necessity of restoring thermodynamic extensivity [14, 15], the restricted phase space formalism was established [16]. In this paradigm, the central charge is introduced as a new thermodynamic variable while the geometric volume is kept fixed, thereby resolving the Euler relation scaling issue. This paradigm enriches the first law and provides a"},{"citing_arxiv_id":"2604.04441","ref_index":57,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravity/thermodynamics correspondence via black hole shadows","primary_cat":"gr-qc","submitted_at":"2026-04-06T05:39:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Cuspy black hole shadows correspond to swallowtail thermodynamic free energy, with boundary self-intersections marking geometric phase transitions whose critical exponents fall in the mean-field class.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"This raises the question of whether an analytical study could produce the similar results. To address this question, we note that the behavior of the cuspy shadow closely resembles the phase transition between small and large black holes. In this context, it is generally observed that r2 > r1, and at the critical point, r2 = r1. Following Ref. [52], we can define the ratio ǫ = 1 − r1 r2 , ǫ ∈ [0, 1). (57) If we can analytically expand these quantities near ǫ = 0, we will obtain the exact exponent. First, let us determine the radii r1 and r2 of the spherical orbits corresponding to the self-intersection point of the shadow boundary. As discussed in Sec. V, there are three methods available; however, obtaining r1 and r2 as analytical functions of a and η (or α ) poses unique challenges. Interestingly, if we substitute r1 with ǫ, such that r1 = (1 − ǫ)r2, these equations can be solved analyti- cally. However, the resulting expressions are quite cum- bersome, and we omit them here. Near ǫ = 0, we perform the following expansions η M 3 = 0 . 7597 − 0. 1778ǫ2 + O(ǫ3), (58) ∆ r M = 1 . 3782ǫ+ 0. 6891ǫ2 + O(ǫ3), (59) for a/M = 1 . 6. At the critical point, we clearly find that ∆ r/M =0 and η/M 3 = 0 . 7597, which corresponds exactly to the critical value of η. Utilizing the expansions mentioned above, we can express ∆ r M = − 3. 2683 ( 0. 7597 − η M 3 ) 1 2 + O ( 0. 7597 − η M 3 ) 3 2 .(60) This confirms the following critical exponent γ = 1 2 , (61) which is consistent with the numerical result from Ref. [45]. Although we have adopted a/M = 1. 6, the exponent remains unchanged for arbitrary values of spin a when 11 0 1 2 3 4 4.6 4.8 5.0 5.2 5.4 5.6 5.8 6.0 r/Slash1M Β/OverTilde /Slash1M (a) ˜α/M =1.8 0 1 2 3 45.0 5.2 5.4 5.6 5.8 6.0 6.2 6.4 r/Slash1M Β/OverTilde /Slash1M (b) ˜α/M =2.11 0 1 2 3 45.0 5.5 6.0 6.5 7.0 r/Slash1M Β/OverTilde /Slash1M (c) ˜α/M =3"},{"citing_arxiv_id":"2603.12524","ref_index":20,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Thermodynamics and information recovery of Schwarzschild AdS black holes in conformal Killing gravity","primary_cat":"gr-qc","submitted_at":"2026-03-12T23:53:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"In conformal Killing gravity, Schwarzschild AdS black holes obey the Bekenstein-Hawking area law, exhibit parameter-dependent Van der Waals-like phase transitions for positive values, and recover information via islands that restore the Page curve after a critical time.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2602.05130","ref_index":50,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Holographic pressure and volume for black holes","primary_cat":"hep-th","submitted_at":"2026-02-04T23:31:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Introduces a holographic pressure and volume for static spherically symmetric black holes via quasi-local thermodynamics, showing large black holes become extensive in the large-system limit while small ones do not.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.12723","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Universal Supercritical Behavior in Global Monopole-Charged AdS Black Holes","primary_cat":"hep-th","submitted_at":"2025-12-14T14:56:16+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Global monopole shifts critical parameters of charged AdS black holes but leaves mean-field universal scaling of Widom line and L± crossover lines unchanged in both ensembles.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.07825","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Novel thermodynamic inequality for rotating AdS black holes","primary_cat":"gr-qc","submitted_at":"2025-12-08T18:54:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A new thermodynamic inequality 4πJ²/(3MV) < 1 is derived for rotating AdS black holes to prevent naked singularities and uphold cosmic censorship.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.01916","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Explicit and covariant formula for thermodynamic volume in extended black hole thermodynamics","primary_cat":"gr-qc","submitted_at":"2025-12-01T17:33:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"An explicit covariant formula for thermodynamic volume is derived that universally decomposes into explicit Lagrangian coupling dependence plus dynamical field response contributions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.21521","ref_index":47,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Synergy between CSST and third-generation gravitational-wave detectors: Inferring cosmological parameters using cross-correlation of dark sirens and galaxies","primary_cat":"astro-ph.CO","submitted_at":"2025-10-24T14:43:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Forecasts that cross-correlating 3G GW dark sirens with CSST photometric galaxies yields 1.04% precision on H0 and 2.04% on Omega_m while also constraining GW clustering bias.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Cao, B. 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Zhang, and X."},{"citing_arxiv_id":"2508.14873","ref_index":38,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Holographic Extended Thermodynamics of deformed AdS-Schwarzschild black hole","primary_cat":"hep-th","submitted_at":"2025-08-20T17:41:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Analyzes bulk and boundary phase transitions in deformed AdS-Schwarzschild black holes using gravitational decoupling and holographic extended thermodynamics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.02716","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Note on Chaos in Hayward Black Holes with String Fluids","primary_cat":"gr-qc","submitted_at":"2025-07-03T15:31:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Melnikov analysis shows charge is essential for chaos under temporal perturbations in Hayward black holes with string fluids while spatial perturbations always produce chaos, with Lyapunov exponents modulated by string density and regularization.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2506.10046","ref_index":105,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"3-dimensional charged black holes in $f({Q})$ gravity","primary_cat":"gr-qc","submitted_at":"2025-06-11T08:00:24+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"New exact charged black hole solutions in (2+1)D f(Q) gravity with cubic form yield a novel AdS solution without GR counterpart, with multiple horizons, stable thermodynamics, and stable photon orbits.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2504.11205","ref_index":39,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing Black Hole Phase Transitions through Quasi-Periodic Oscillations","primary_cat":"gr-qc","submitted_at":"2025-04-15T14:07:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"QPO frequencies in RN AdS and Kerr geometries trace distinct thermodynamic phases and their stability when plotted against Hawking temperature.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1608.06147","ref_index":73,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Black hole chemistry: thermodynamics with Lambda","primary_cat":"hep-th","submitted_at":"2016-08-22T12:32:49+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Treating the cosmological constant as pressure in black hole thermodynamics yields an extended dictionary with enthalpy, thermodynamic volume, and chemical-like phase transitions including Van der Waals behavior, reentrant transitions, and triple points.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"17The fact that this ratio has no dependence on black hole charge Q is unsurprising by dimensional arguments. However, there is currently no obvious explanation as to why both ratios are the same. This is true, however, only in four dimensions-for charged-AdS black holes in higher dimensions the ratio becomes Pcvc/Tc = (2d− 5)/(4d− 8) [141]. - 27 - exponents18 [73]: α = 0 , β = 1 2 , γ = 1 , δ = 3 . (4.18) An example of black holes with a critical point characterized by different critical expo- nents is given in Sec. 4.5. The coexistence line is governed by the behavior of the Gibbs free energy (the bottom line of the swallowtail). Alternatively, it can be obtained [142] by imposing Maxwell's equal area law , which states that the two phases coexist when the areas"}],"limit":50,"offset":0}