{"total":11,"items":[{"citing_arxiv_id":"2606.28853","ref_index":23,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological structure growth in energy-momentum squared gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-06-27T10:26:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"In f(R,T²) gravity, the growth index decreases with redshift and approaches standard matter-dominated values at early times, with fσ8 predictions staying within ±2σ observational bounds for viable coupling parameters α and n=1/2 or 1/4.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27441","ref_index":24,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Collider Probes of Dark Energy Microphysics","primary_cat":"hep-ph","submitted_at":"2026-06-25T18:03:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Collider observables of a pseudoscalar mediator resonance can become sensitive to the sound speed of dark energy fluctuations via modified propagation in a dark energy background.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22434","ref_index":47,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Entropic route to Brown-York tensor: A unified framework for null and timelike hypersurfaces","primary_cat":"gr-qc","submitted_at":"2026-05-21T12:59:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"An entropy functional yields the Brown-York tensor via conjugate momentum projection, unifying null and timelike hypersurfaces and reproducing equations in scalar-tensor gravity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22348","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark Energy in Ghost-free non-local Gravity","primary_cat":"gr-qc","submitted_at":"2026-05-21T11:34:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Ghost-free non-local gravity fits Pantheon+, DESI, and H(z) data but fails with added CMB, while generalized exponential F(R) gravity outperforms Lambda CDM across all datasets including CMB.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.10992","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Photon Sphere and Shadow of a Perturbative Black Hole in $f(R,\\mathcal{G})$ Gravity","primary_cat":"gr-qc","submitted_at":"2026-05-09T12:16:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Perturbative f(R,G) corrections shift the photon-sphere radius and shadow size, with the Gauss-Bonnet term dominating over mixed curvature contributions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.23564","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Energy conditions of bouncing solutions in quadratic curvature gravity coupled with a scalar field","primary_cat":"gr-qc","submitted_at":"2026-03-24T07:53:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bouncing solutions in quadratic curvature gravity with a scalar field satisfy null, weak, and dominant energy conditions but violate the strong one when using the scalar-field energy-momentum tensor, while all four conditions are violated near the bounce in the effective tensor formulation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.10850","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"F(R,..) theories from the point of view of the Hamiltonian approach: non-vacuum Anisotropic Bianchi type I cosmological model","primary_cat":"gr-qc","submitted_at":"2025-12-11T17:39:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Classical solutions for F(R) gravity in Bianchi type I cosmology with barotropic matter are derived via the Hamiltonian formalism in two gauges.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.08638","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Interacting bosonic dark energy and fermionic dark matter in Einstein scalar Gauss-Bonnet gravity","primary_cat":"astro-ph.CO","submitted_at":"2025-08-12T05:03:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Models of interacting bosonic dark energy and fermionic dark matter in Einstein-scalar-Gauss-Bonnet gravity with exponential and power-law potentials are dynamically analyzed and constrained by observational data, showing consistency with LambdaCDM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.05207","ref_index":63,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Interacting Scalar Fields as Dark Energy and Dark Matter in Einstein scalar Gauss Bonnet Gravity","primary_cat":"gr-qc","submitted_at":"2025-07-07T17:16:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Interacting scalar fields coupled to Gauss-Bonnet gravity yield viable dark energy and dark matter models that match Pantheon+ and DES supernova data while preferring over LambdaCDM at high redshifts with Roman mocks.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"gravity: Why, how and what?, Gen. Rel. Grav. 54, 44 (2022), arXiv:2204.06533 [gr-qc]. [61] T. P. Sotiriou and V. Faraoni, f(R) Theories Of Gravity, Rev. Mod. Phys. 82, 451 (2010), arXiv:0805.1726 [gr-qc]. [62] S. Nojiri and S. D. Odintsov, Introduction to modified gravity and gravitational alternative for dark energy, eConfC0602061, 06 (2006), arXiv:hep-th/0601213. [63] R.-J. Yang, New types of 𝑓 (𝑇) gravity, Eur. Phys. J. C71, 1797 (2011), arXiv:1007.3571 [gr-qc]. [64] F. K. Anagnostopoulos, S. Basilakos, and E. N. Saridakis, First evidence that non-metricity f(Q) gravity could challenge ΛCDM, Phys. Lett. B 822, 136634 (2021), arXiv:2104.15123 [gr-qc]. [65] O. Sokoliuk, S. Arora, S. Praharaj, A. Baransky, and P."},{"citing_arxiv_id":"1907.08010","ref_index":100,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological searches for the neutrino mass scale and mass ordering","primary_cat":"astro-ph.CO","submitted_at":"2019-07-18T12:03:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Thesis summarizing an upper limit of 0.12 eV on the neutrino mass sum, bias calibration via CMB lensing cross-correlations, and tighter limits plus stronger normal-ordering preference in non-phantom dynamical dark energy models.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"of temperature anisotropies in the CMB, provided strong support for the existence of the DM already theorized by Zwicky in the 1930s. By the end of the 1990s, two independent groups led by Riess and Perlmutter used Type Ia Supernovae (SNeIa) to demonstrate that the Universe is accelerating [96,97], thus requiring some form ofdark energy(DE), possibly in the form of a cosmological constantΛ [98,99], or requiring modifications of gravity [100-104]. Besides CMB and SNeIa, a number of other observational probes began flourishing espe- cially in the early 2000s. A special mention goes to probes of the large-scale structure (LSS), particularly galaxy redshift surveys. A crucial role in the development of galaxy redshift surveys was played by the Sloan Digital Sky Survey (SDSS) [105]: in 2005, SDSS was the"},{"citing_arxiv_id":"1705.11098","ref_index":73,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Modified Gravity Theories on a Nutshell: Inflation, Bounce and Late-time Evolution","primary_cat":"gr-qc","submitted_at":"2017-05-31T13:41:52+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Modified gravity theories supply viable mathematical frameworks for inflation, bounces, and dark energy eras that match observational data.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"MODIFIED GRA VITIES AND COSMOLOGY A. F (R) Gravity The theory of F (R) gravity could be considered as the most popular among modified gra vity theories. In this section, a general review of the F (R) gravity theory is given. In the literature there are various review s also discussing this topic, see [62, 72-75, 77, 78]. 8 1. General properties The action of the F (R) gravity [73] is given by replacing the scalar curvature R in the Einstein-Hilbert action which is,1 SEH = ∫ d4x√ −g ( R 2κ 2 + Lmatter ) , (1) by using some appropriate function of the scalar curvature, as fo llows, SF (R) = ∫ d4x√ −g (F (R) 2κ 2 + Lmatter ) . (2) ndequation In Eqs. (1) and (2), Lmatter is the matter Lagrangian density. We now review in brief the general properties"}],"limit":50,"offset":0}