{"total":11,"items":[{"citing_arxiv_id":"2605.18186","ref_index":10,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Case for Astrons","primary_cat":"gr-qc","submitted_at":"2026-05-18T10:27:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"UNKNOWN","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A sparse population of primordial charged compact objects is hypothesized with specific parameters and shown to face severe plasma-screening and neutralization constraints while failing to produce late-time acceleration in the homogeneous FLRW approximation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.03428","ref_index":75,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Families of regular spacetimes and energy conditions","primary_cat":"gr-qc","submitted_at":"2026-05-05T07:10:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A classification of admissible energy density profiles with bounded Kretschmann scalar yields a unified framework for regular static spherically symmetric spacetimes satisfying the weak energy condition, recovering known models and producing new families with hypergeometric and other closed forms.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Tab =T µνeaµebν = diag(ρ, p1, p2, p3),(2.16) whereρdenotes the total density of mass-energy,p 1 the radial pressure,p2 andp 3 the tan- gential pressures [11, 79], and eaµ = ( diag h 1/ √ B, √ B,1/r,1/(rsinθ) i ,(B >0), diag \u0002 1/ √ −B, √ −B,1/r,1/(rsinθ) \u0003 ,(B <0), (2.17) which is a standard result for the geometry (2.1). In this way, the classical energy relations (2.9)-(2.12) read as [78] NEC⇔ρ+p i ≥0, WEC⇔ρ≥0, ρ+p i ≥0, SEC⇔ρ+ X i pi ≥0, ρ+p i ≥0, DEC⇔ρ≥0, ρ≥ |p i|, (2.18a) (2.18b) (2.18c) (2.18d) for alli= 1,2,3. We note that the diagonalization of the energy-momentum tensor may break down at a (Killing) horizonr=r h (whereB(r h) = 0), sincee aµ becomes singular. Nevertheless, the energy conditions at the horizon can be obtained as the limitr→r h of"},{"citing_arxiv_id":"2605.02813","ref_index":71,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Derivation of the Smarr formula from the Komar charge in Einstein-nonlinear electrodynamics theories and applications to regular black holes","primary_cat":"gr-qc","submitted_at":"2026-05-04T16:49:43+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"In our conventions, the energy conditions [70] are defined in Table2. Name Statement Conditions Weak (WEC) Tµν vµ vν ≤0 ρ≥0,ρ+p i ≥0 Null (NEC) Tµν kµ kν ≤0 ρ+p i ≥0 Strong (SEC) Tµν − 1 2 T gµν \u0001 vµ vν ≤0 ρ+p i ≥0,ρ+ ∑i pi ≥0 Dominant (DEC) Sµ ≡ −T µ νvν (future-directed) ρ≥0,ρ≥ |p i| Table2: Energy conditions in our conventions. The results for the Bardeen solution [71] are collected in Table3. The null energy condition (NEC) and the weak energy condition (WEC) are satisfied everywhere, while the strong energy condition (SEC) holds only for radiir> q 2c 3 . This behaviour is expected from the Penrose-Hawking singularity theorems [72,73]: 17 since the Bardeen solution is regular, the SEC must be violated in the region where a singularity would"},{"citing_arxiv_id":"2604.21014","ref_index":40,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"3D near-de Sitter gravity and the soft mode of DSSYK","primary_cat":"hep-th","submitted_at":"2026-04-22T19:01:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The soft mode of DSSYK is dual to 3D near-de Sitter gravity with a localized dS2 slice, where effective actions, entropies, and correlators match via conformal boundary conditions on future and past infinity.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"1 Boundary conditions To make the gravitational dynamics uniquely defined, we need to fix boundary conditions at past and future infinityI ˘, and on the gluing surface Σ. AtI ˘, we choose conformal boundary conditions that fix the conformal structure of the metric and the trace of the extrinsic curvature. These boundary conditions are standard in (A)dS/CFT (see, e.g. [40, 41, 42]). Defineσ ij \"e ωpxiqˆσij, and introduce a Fefferman-Graham-like expansion for the boundary metric and the trace of the extrinsic curvature ˆσij \"e 2T ˆσp0q ij `ˆσp2q ij `. . . TÑ 8.(51) Kσ \"K p2q σ `e '2T Kp4q σ `. . . In near-de Sitter gravity, we choose ˆσp0q ij \"δ ij, K p4q σ \"4. (52) There are good reasons to believe that fixing the leading term of the metric ˆσ p0q"},{"citing_arxiv_id":"2604.16545","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Energy conditions in static, spherically symmetric spacetimes and effective geometries","primary_cat":"gr-qc","submitted_at":"2026-04-17T06:08:58+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"In this section, we perform a detailed examination of classical energy conditions in the most general static and spherically symmetric spacetime ds2 =g µνdxµdxν =−B(r)dt 2 +A(r)dr 2 +r 2dΩ2 ,(2.1) withdΩ 2 = dθ2 + sin2 θdϕ 2 the line element on the two-sphere. Energy criteria are most conveniently discussed in the local proper reference frame (ˆt,ˆr, ˆθ, ˆϕ) of a static observer [4, 19]. For this reason, we introduce the non-coordinate orthonormal basis in the standard manner [54, 55]: ea =e aµ (∂/∂x µ),(2.2a) with the dual basis fulfilling ea =e aµdxµ ,(2.2b) - 3 - where Latin indicesa, b,· · ·= ˆ0, ˆ1, ˆ2, ˆ3denote frame components, Greek indices correspond to coordinate components, ande aµ represents the inverse ofeaµ. These objects, referred"},{"citing_arxiv_id":"2511.19582","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"On Modelling the Surfaces of Celestial Bodies in Quantum Gravity","primary_cat":"gr-qc","submitted_at":"2025-11-24T18:52:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A modified Tolman VII density profile with sufficient differentiability produces regular quantum corrections to stellar exteriors when computed with the Vilkovisky-DeWitt effective action.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.05700","ref_index":49,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Entanglement Entropy and Thermodynamics of Dynamical Black Holes","primary_cat":"hep-th","submitted_at":"2025-09-06T12:32:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"In f(R) theories, the replica-method gravitational entropy computed on the apparent horizon matches the Hollands-Wald-Zhang dynamical black hole entropy and satisfies the first law, while the event horizon does not; this lets the generalized second law be reinterpreted as matter entanglement across ","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.09202","ref_index":31,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Angular momentum of vacuum bubbles in a first-order phase transition","primary_cat":"hep-ph","submitted_at":"2025-05-14T07:28:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Computes the dimensionless spin parameter s = J/(G_N M^2) of false vacuum bubbles from density and velocity perturbations in FOPTs, yielding values from O(10^{-5}) to O(10) and a scaling relation with FOPT timescale, wall velocity, and temperature ratio.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2404.13332","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Redundancy of the cosmological evolution equations and its relationship with the initial conditions","primary_cat":"gr-qc","submitted_at":"2024-04-20T09:41:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Redundancy of cosmological evolution equations in FLRW models is inevitable in general relativity and accounts for the special role of one Friedmann equation in constraining initial values.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2303.11713","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The physics of gravitational waves","primary_cat":"gr-qc","submitted_at":"2023-03-21T10:04:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"Lecture notes deriving gravitational wave physics from first principles in general relativity for PhD and advanced MSc students.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2109.01398","ref_index":224,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Scalar induced gravitational waves review","primary_cat":"gr-qc","submitted_at":"2021-09-03T09:44:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review that unifies analytical expressions for scalar-induced gravitational waves and emphasizes calculations for non-radiation-dominated cosmologies.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"where R(3)[Yij] and Di are respectively the 3D Ricci scalar and the covariant derivative associated toYij. Since we work in Cartesian coordinates, we already used thatdetY = 1. In going from (3.3) to (3.4) we took a big leap in the (3+1) and conformal decomposition of the 4D Ricci scalar. Some steps can be found in App. C. For more details, the interested reader is referred to E. Poisson's book [223] for the (3+1) or ADM decomposition [224], and to the appendix of R. Wald's book [225] for the conformal transformation rules. Now, we could take the variation of (3.4) with respect toYij, having in mind that the result should still be transverse and traceless, and obtain the transverse-traceless spatial component of Einstein Equations. However, this would not be very illuminating. Before taking the variation, let"}],"limit":50,"offset":0}