{"total":13,"items":[{"citing_arxiv_id":"2605.20227","ref_index":10,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Cosmological perturbations with $f(R)$ gravity scalarons : Galaxy power spectra and the scalaron mass","primary_cat":"astro-ph.CO","submitted_at":"2026-05-15T08:22:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"In a viable f(R) model transitioning from early GR-like to late non-GR behavior, matter power spectra show higher monopole and quadrupole power at small scales with quadrupole elevated at large scales up to k~0.02, while scalaron mass decreases over time to GR limits on galactic scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13914","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Amplitude-Growth Degeneracy and Implied $A_s$ Diagnostic for Background-Inert Modified Gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T09:41:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Any background-inert λ in coincident f(Q) gravity degenerates with σ80 via an As-D0(λ) link, inflating σ80 to unphysical levels and raising As by 20-30% in tension with Planck unless fixed by As priors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12003","ref_index":33,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Generalized Mass-to-Horizon Entropy and Horizon Thermodynamics","primary_cat":"gr-qc","submitted_at":"2026-05-12T11:53:41+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":"To examine the thermodynamic behavior of the system, we analyze the evolution of the first and second derivatives of the generalized mass-to-horizon entropy using the modified Friedmann equation obtained in the previous section. It is well known that any thermodynamic system must evolve to a state of maximum entropy corresponding to its equilibrium state. Such an evolution must satisfy two important conditions[33, 34], ˙S≥0, ¨S <0,(20) where the dots represent derivatives with respect to cosmic time. The first condition implies that the entropy always increases throughout the evolution of the system, whereas the second condition implies that the entropy approaches 7 a maximum value asymptotically, corresponding to the equilibrium state of the system[34]. We need to check the"},{"citing_arxiv_id":"2605.10965","ref_index":44,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Constraining Dark Energy Dynamics in Curved Spacetime with Current Observations","primary_cat":"physics.gen-ph","submitted_at":"2026-05-08T10:57:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Observational constraints on a dark energy EoS parametrization in curved spacetime yield α ≈ 0.35 (0.56) and Ω_k0 that changes sign with ANN data reconstruction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04123","ref_index":21,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Testing an anisotropic spinor field--based Modified Chaplygin Gas model in Kantowski--Sachs spacetime with observational constraints","primary_cat":"gr-qc","submitted_at":"2026-05-05T13:46:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"A spinor-field Modified Chaplygin Gas model in Kantowski-Sachs spacetime yields H0 of 67-68 km/s/Mpc, late-time isotropy, q0 of -0.49, and a better AIC fit than LambdaCDM.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"3847/1538-4357/acbfb8, arXiv:2208.08512. [18] DESI Collaboration, Mon. Not. R. Astron. Soc.522, 2038 (2023), doi:10.1093/mnras/stad1136, arXiv:2306.06308. [19] DESI Collaboration et al.,(2025), https://doi.org/10.48550/arXiv.2503.14745. [20] DESI Collaboration et al., Phys. Rev. D112, 083515 (2025), https://doi.org/10.1103/tr6y- kpc6, arXiv:2404.03000. [21] S. Weinberg, Rev. Mod. Phys.61, 1 (1989), doi:10.1103/RevModPhys.61.1. [22] S. M. Carroll, Living Rev. Relativ.4, 1 (2001), doi:10.12942/lrr-2001-1, arXiv:astro- ph/0004075. [23] A. G. Riesset al., Astrophys. J.876, 85 (2019), doi:10.3847/1538-4357/ab1422, arXiv:1903.07603. [24] L. Verde, T. Treu and A. G. Riess, Nature Astron.3, 891 (2019), doi:10."},{"citing_arxiv_id":"2604.22450","ref_index":7,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Exploring Cosmic Evolution in R\\'enyi Entropic Cosmology with Constraints from DESI DR2 BAO and GW Data","primary_cat":"gr-qc","submitted_at":"2026-04-24T11:08:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Rényi entropic corrections to cosmology are constrained by DESI DR2 BAO and GW data to a viable quintessence-like model that approaches ΛCDM without phantom behavior and satisfies BBN bounds.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"from various eras has been shown by this hypothesis. Nevertheless, theΛCDM framework has a number of serious conceptual problems even with its practical effectiveness. The most well-known of these is the cosmological constant issue, which results from the huge difference between the observed and theoretically expected levels of vacuum energy density[7, 8]. Further challenging our comprehension are the fine-tuning and cosmic coincidence problems [7, 9, 10], which ask why the current value of dark energy density is so perfectly tuned and why its dominance corresponds with the current period of cosmic evolution. Such theoretical challenges shows the need for the exploration of other theoret- ical possibilities causing the late-time cosmic acceleration, outside the domain of standardΛCDM paradigm."},{"citing_arxiv_id":"2604.21151","ref_index":6,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The $f(Q, T)$ gravity and affine EoS: observational aspects","primary_cat":"gr-qc","submitted_at":"2026-04-22T23:30:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"f(Q,T) gravity with linear form and affine EoS is constrained by CC, Pantheon+SH0ES and DESI BAO data, yielding a present universe age consistent with Planck within 1σ.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"641, A6 (2020) https://doi.org/10.1051/0004-6361/201833910 [4] V . Sahni and A. Starobinsky, The case for a positive cosmo logical Λ -term, Int. J. Mod. Phys. D 9, 373 (2000) https://doi.org/10.1142/S0218271800000542 [5] T. Padmanabhan, Cosmological constant-the weight of th e vacuum, Phys. Rep. 380, 235 (2003) https://doi.org/10.1016/S0370-1573(03)00120-0 [6] S. Weinberg, The cosmological constant problem, Rev. Mo d. Phys. 61, 1 (1989) https://doi.org/10.1103/RevModPhys.61.1 [7] P . J. Steinhardt, L. Wang, and I. Zlatev, Cosmological tr acking solutions, Phys. Rev. D 59, 123504 (1999) https://doi.org/10.1103/PhysRevD.59.123504 13 [8] E. Di V alentino, et al., In the realm of the Hubble tension -a review of solutions, Class."},{"citing_arxiv_id":"2604.17017","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Transiently accelerating cosmological model with Gong-Zhang parametrization in $f(T)$ teleparallel gravity","primary_cat":"gr-qc","submitted_at":"2026-04-18T14:56:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"In f(T) gravity with Gong-Zhang EoS parametrization, the fitted model shows transient acceleration followed by future deceleration and satisfies thermodynamic consistency.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"pothesis of dark energy (DE), a dominant component believed to be responsible for driving this late-time acceleration. Despite its substantial contribution to the total energy density of the universe, the fundamental nature of DE remains a mysterious problem in modern cosmolog y. Observational evidence indicates that dark energy together with dark matter, constitutes approximate ly 95 - 96% of the total cosmic energy content [4]. Among the various candidates proposed for DE, the cosmologi cal constant ( Λ ) stands out as the simplest and most successful model. The standard Λ CDM framework provides an excellent agreement with current ob- servational data. However, it suffers from two major theore tical challenges, namely the fine-tuning problem and the coincidence problem [5-8]."},{"citing_arxiv_id":"2604.04687","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Natural SUSY with mixed axion/axino dark matter","primary_cat":"hep-ph","submitted_at":"2026-04-06T13:53:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Natural SUSY with axino LSP allows viable mixed axion-axino dark matter matching the observed abundance for axino masses near 100 keV and PQ scales of 10^11 to 3x10^12 GeV in DFSZ and KSVZ models.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"problem (why is the CP-violating QCD Lagrangian contribution to the neutron electric dipole moment (EDM) so tiny) and the cosmological constant problem (why is the spacetime vacuum energy density over 120 orders of magnitude smaller thanM 4 P lanck?). While the latter might be solved in the context of anthropic selection in an eternally inflating multiverse [1, 2], the most promising solution to the first is softly broken supersymmetry [3] (SUSY) while the strong CP problem is solved by the Peccei-Quinn (PQ) mechanism and its concomitantaxion[4-6]. While SUSY is adept at stabilizing the weak scale, thus solving the big hierarchy problem, the apparent lack of superpartners at the LHC (so far) has seemingly engendered a little hier-"},{"citing_arxiv_id":"2603.18223","ref_index":105,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Gamma-Ray Bursts as an Independent High-Redshift Probe of Dark Energy","primary_cat":"astro-ph.CO","submitted_at":"2026-03-18T19:14:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Forecasts show that ~66 optical GRBs can achieve σ_w ≈ 0.47 in wCDM using Dainotti relations, matching Planck precision and enabling independent high-redshift tests of dark energy.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The flatΛCDM model successfully fits observations such as the Cosmic Microwave Background (CMB) radiation (N. Aghanim et al. 2020a), the Baryon Acoustic Oscillations (BAO; S. Alam et al. 2021), and the accelerated expansion of the Universe inferred from Type Ia Supernovae (SNe Ia). Nevertheless, it presents well-known theoretical shortcomings. One example is the cosmological constant problem (S. Weinberg 1989), which reflects the discrepancy between the expected and the observed values ofΩΛ, as well as the unresolved question of the physical origin of Dark Energy. Another issue is the fine-tuning (or coincidence) problem, which arises from the fact that the current values of the matter density (ΩM) and the Dark Energy density (ΩΛ) are of the same order"},{"citing_arxiv_id":"2602.08562","ref_index":15,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Evolutionary Phase of Universe in $f(R,L_m,T)$ Gravity: The Dynamical System Analysis","primary_cat":"gr-qc","submitted_at":"2026-02-09T12:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Dynamical systems analysis in f(R,L_m,T) gravity identifies stable critical points that describe different evolutionary phases of the Universe.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.24339","ref_index":16,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"de Sitter Corrections to Gravitational Wave Memory","primary_cat":"gr-qc","submitted_at":"2025-09-29T06:39:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The paper derives leading-order de Sitter corrections of order Lambda to gravitational wave displacement and spin memory using an adapted Bondi-Sachs framework.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.11839","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Classical Planck Spectrum for Relative Thermal Radiation, Classical Zero-Point Radiation, and Scale Parameter","primary_cat":"physics.class-ph","submitted_at":"2019-07-27T02:59:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Claims classical derivation of Planck spectrum via scale parameter for zero-point radiation in cavities, with parameter value order of h.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}