{"total":13,"items":[{"citing_arxiv_id":"2605.26259","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Charging Across the Phantom Divide with Modified Gravity","primary_cat":"gr-qc","submitted_at":"2026-05-25T18:38:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Horndeski gravity with shift symmetry and linear potential permits three mechanisms for crossing the phantom divide but none fit current data well without a cosmological constant.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.26116","ref_index":219,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Unifying Early and Late Dark Energy: Dynamical Requirements and Obstructions","primary_cat":"astro-ph.CO","submitted_at":"2026-05-25T17:59:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Any unified early and late dark energy scenario with a single tracking scalar field requires a potential with three distinct slopes arranged in a steep-steeper-shallow hierarchy.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Zhang, T.-N. Li, G.-H. Du, S.-H. Zhou, L.-Y. Gao, J.-F. Zhang et al.,Alleviating the H0 tension through new interacting dark energy model in light of DESI DR2,2510.12627. - 38 - [218] M. Yashiki,Toward a simultaneous resolution of the H0 and S8 tensions: Early dark energy and an interacting dark sector model,Phys. Rev. D112(2025) 063517 [2505.23382]. [219] E. Silva, M.A. Sabogal, M. Scherer, R.C. Nunes, E. Di Valentino and S. Kumar,New constraints on interacting dark energy from DESI DR2 BAO observations,Phys. Rev. D111 (2025) 123511 [2503.23225]. [220] M. Tsedrik et al.,Interacting dark energy constraints from the full-shape analyses of BOSS DR12 and DES Year 3 measurements,2502.03390. [221] M.A. Sabogal, E."},{"citing_arxiv_id":"2605.26173","ref_index":65,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Effect of $R^2$ on the stability of de Sitter solution of the generalized Einsteinian cubic gravity","primary_cat":"physics.gen-ph","submitted_at":"2026-05-25T04:28:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Generalized Einsteinian cubic gravity admits a de Sitter solution from the P cubic term alone; stability analysis is incomplete until the R^2 term is added, which leaves the solution value unchanged.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18240","ref_index":10,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Phase-Space Analysis of Quadratic Dark Energy: Stable Attractors and Their Observational Signatures","primary_cat":"astro-ph.CO","submitted_at":"2026-05-18T11:34:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Phase-space analysis of a quadratic dark energy model identifies stable attractors that approach the phantom divide asymptotically from both sides without crossing it.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.06147","ref_index":8,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cosmological Dynamics of a Non-Canonical Generalised Brans-Dicke Theory","primary_cat":"gr-qc","submitted_at":"2026-05-07T12:41:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A non-canonical generalized Brans-Dicke theory admits background cosmological solutions matching Lambda CDM characteristics for constant, power-law, and exponential potentials, with dynamics distinct from other scalar-tensor models.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"time accelerated cosmic expansion. Moreover, the contri- bution of cosmic inflation provides a suitable initial point from which this dynamics evolves from the early primor- dial Universe to its present state [7]. Despite the attrac- tive feature of this dynamical background, the cosmolog- ical constant is well known to have internal consistency problems [8], and the potential direct detection of CDM particles remains elusive [9] despite great efforts. The robustness in the measurement of cosmological param- eter has led to the appearance of cosmological tensions in recent years [1, 10-12] which has led to a plethora of potential new physics settings beyond ΛCDM [2, 13]. On the other hand, these different cosmologies produce dif-"},{"citing_arxiv_id":"2605.05122","ref_index":22,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Exponential Quintessence: Analytic Relationship Between the Current Equation of State Parameter and the Potential Parameter","primary_cat":"astro-ph.CO","submitted_at":"2026-05-06T16:51:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"For an exponential quintessence potential, an analytic formula links the current equation-of-state w_φ0 to the potential slope λ while enforcing prior radiation and matter domination, yielding the bound λ < 1.94 at Ω_φ0 = 0.685.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Sava¸ s Arapo˘ glu and A. Emrah Y¨ ukselci, Dynamical System Analysis of Quintessence Models with Exponential Potential - Revisited, Mod. Phys. Lett. A34, 1950069 (2019), arXiv:1711.03824 [gr-qc]. [21] D. Andriot, S. Parameswaran, D. Tsimpis, T. Wrase, and I. Zavala, Exponential quintessence: curved, steep and stringy?, JHEP08, 117, arXiv:2405.09323 [hep-th]. [22] G. Obied, H. Ooguri, L. Spodyneiko, and C. Vafa, De Sitter Space and the Swampland (2018), arXiv:1806.08362 [hep-th]. [23] M. Nitta and K. Uzawa, Dynamical de Sitter conjecture and quintessence model (2025), arXiv:2501.02258 [hep-th]. [24] M. Cicoli, J. P. Conlon, A. Maharana, S. Parameswaran, F. Quevedo, and I. Zavala, String cosmology: From the early universe to today, Phys."},{"citing_arxiv_id":"2603.21125","ref_index":49,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Model-Independent Reconstruction of Quintessence Potential and Kinetic Energy from DESI DR2 and Pantheon+ Supernovae","primary_cat":"astro-ph.CO","submitted_at":"2026-03-22T08:46:57+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Quintessence potential decreases monotonically with redshift while kinetic energy crosses zero near z=1, with negative values at intermediate redshifts being statistical artifacts from derivative reconstruction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2602.19118","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Exponential Quintessence Model: Analytical Quantification of the Fine-Tuning Problem in Dark Energy","primary_cat":"astro-ph.CO","submitted_at":"2026-02-22T10:25:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Exponential quintessence with an assumed kination epoch relaxes the dark energy fine-tuning problem by dozens of orders of magnitude relative to a cosmological constant.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.19154","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dynamical system analysis of the cosmological phases in Palatini $k$-essence gravity","primary_cat":"gr-qc","submitted_at":"2025-11-24T14:23:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Dynamical systems analysis of a Palatini k-essence model identifies fixed points for quasi-de-Sitter epochs, scaling solutions, and quintessence phases connected by heteroclinic orbits in flat FLRW cosmology.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.09467","ref_index":64,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting the Hubble tension problem in the framework of holographic dark energy","primary_cat":"astro-ph.CO","submitted_at":"2025-11-12T16:39:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"HDE models with future event horizon IR cutoff partially ease the Hubble tension while Hubble-scale cutoffs do not, consistent across six models and multiple BAO/SN/CMB combinations.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"one can identify the general features of HDE models that provide better fits to the data. Therefore, in this work, we systematically investigate the Hubble tension problem based on all four categories of HDE models. Specifically, we select one or two representative models from each cat- egory, as summarized in Table I. For the first category, we consider the original HDE (OHDE) model [64]. For the second category, we analyze the generalized Ricci HDE (GRDE) model [70]. For the third category, we examine two interacting HDE models: IHDE1 [72], which uses the Hubble scale as the IR cutoff, and IHDE2 [73], which uses the future event horizon as the IR cutoff. For the fourth category, we study the Tsallis HDE (THDE) model [77] and Barrow HDE (BHDE) model [78], where THDE em-"},{"citing_arxiv_id":"2509.09202","ref_index":85,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Interacting $k$-essence field with non-pressureless Dark Matter: Cosmological Dynamics and Observational Constraints","primary_cat":"astro-ph.CO","submitted_at":"2025-09-11T07:18:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Interacting k-essence dark energy and non-pressureless dark matter models with two interaction forms are shown to reproduce major cosmological epochs and fit observations comparably to LambdaCDM while admitting late-time de Sitter attractors.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"10604 [gr-qc]. [83] P. Jorge, J. P. Mimoso, and D. Wands, On the dynamics of k-essence models, J. Phys. Conf. Ser.66, 012031 (2007). [84] S. Bahamonde, C. G. B ¨ohmer, S. Carloni, E. J. Copeland, W. Fang, and N. Tamanini, Dynamical systems applied to cos- mology: dark energy and modified gravity, Phys. Rept.775- 777, 1 (2018), arXiv:1712.03107 [gr-qc]. [85] M. Bouhmadi-L 'opez, J. Marto, J. Morais, and C. M. Silva, Cosmic infinity: A dynamical system approach, JCAP03, 042, arXiv:1611.03100 [gr-qc]. [86] A. Alho, C. Uggla, and J. Wainwright, Dynamical systems in perturbative scalar field cosmology, Class. Quant. Grav.37, 225011 (2020), arXiv:2006.00800 [gr-qc]. [87] S. Das, M. Banerjee, and N. Roy, Dynamical System Analysis"},{"citing_arxiv_id":"2509.02539","ref_index":37,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Extending the Dynamical Systems Toolkit: Coupled Fields in Multiscalar Dark Energy","primary_cat":"hep-th","submitted_at":"2025-09-02T17:41:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"New dynamical systems variables for coupled axion-saxion fields yield a general non-geodesicity expression at fixed points and identify genuinely non-geodesic attractors under exponential couplings.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1906.08920","ref_index":46,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmology in symmetric teleparallel gravity and its dynamical system","primary_cat":"gr-qc","submitted_at":"2019-06-21T02:21:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"In f(Q) symmetric teleparallel gravity, accelerating expansion is geometric; dynamical analysis of f(Q)=Q+αQ² yields five critical points with stable de Sitter (P4) and matter-dominated (P5) attractors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}