{"total":15,"items":[{"citing_arxiv_id":"2606.24131","ref_index":36,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Minimal Extensions of the $\\alpha$-Starobinsky Model: Reconciling ACT DR6 and Reheating Constraints","primary_cat":"astro-ph.CO","submitted_at":"2026-06-23T04:31:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Two minimal single-parameter extensions of the α-Starobinsky model shift ns into the 1σ ACT DR6 region while keeping r < 0.038 and yielding T_re ~ 10^9 GeV for N_k in [50,65].","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19513","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reheating as a variational probe of cosmological observables","primary_cat":"astro-ph.CO","submitted_at":"2026-06-17T18:55:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Reheating is formulated as a regularized variational problem in equation-of-state space whose extremal histories are selected by different cosmological observables.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12549","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tachyonic Encore: A universal shift of inflationary observables","primary_cat":"hep-th","submitted_at":"2026-06-10T18:01:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A light axion spectator induces post-inflation tachyonic phases that produce a nearly scale-invariant boost to the curvature power spectrum and alter key inflationary observables in a largely potential-independent manner.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12519","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Observing Cosmic Reheating with the expanded Simons Observatory","primary_cat":"astro-ph.CO","submitted_at":"2026-06-10T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Expanded Simons Observatory could measure reheating temperature and inflaton-gluon coupling to a few percent in QCD-driven warm inflation if r=0.01 primordial gravitational waves are found.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19825","ref_index":82,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Inflaton Accretion onto Primordial Black Holes During Reheating","primary_cat":"astro-ph.CO","submitted_at":"2026-05-19T13:18:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Inflaton accretion during reheating drives non-linear PBH mass growth that extends lifetimes and amplifies emitted SGWB by multiple orders of magnitude.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18641","ref_index":24,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Inflation from a Weyl-flat null origin","primary_cat":"hep-ph","submitted_at":"2026-04-19T14:50:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Single-field inflation with ε(N) approaching a constant in (0,1) at early times forms an asymptotic universality class with a Weyl-flat null origin while producing ns and r values compatible with Planck data.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the viable corridor and incorporate reheating-aware pivot matching, which separates points that merely fall within the CMB ellipse from those that also admit a conventional thermal history [20-23]. In this respect the framework is naturally aligned with recent studies that connect inflationary dynamics and post-inflationary sectors while retaining predictive control over late-time observables [24, 25]. The resulting class ofasymptotically Weyl-flat inflationary modelsconsists of canonical Einstein-scalar backgrounds that are power-law and Weyl-flat in the far past, phenomenolog- ically acceptable in the observable window, and smoothly terminating at finiteN. The scope is correspondingly specific. We do not derive the quantum state from first principles, nor"},{"citing_arxiv_id":"2604.16085","ref_index":41,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Thermal effects on Dark Matter production during cosmic reheating","primary_cat":"hep-ph","submitted_at":"2026-04-17T14:14:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Thermal corrections to reheating and freeze-in DM production rates are generally small in the computable regime but can be large in constructed counter-examples.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Loeb,Inflation and the Scale Dependent Spectral Index: Prospects and Strategies,JCAP02(2011) 021 [1007.3748]. [39] J. Mielczarek,Reheating temperature from the CMB,Phys. Rev. D83(2011) 023502 [1009.2359]. [40] R. Easther and H.V. Peiris,Bayesian Analysis of Inflation II: Model Selection and Constraints on Reheating,Phys. Rev. D85(2012) 103533 [1112.0326]. [41] L. Dai, M. Kamionkowski and J. Wang,Reheating constraints to inflationary models,Phys. Rev. Lett.113(2014) 041302 [1404.6704]. [42] M. Drewes,What can the CMB tell about the microphysics of cosmic reheating?,JCAP03 (2016) 013 [1511.03280]. [43] J. Ghiglieri and M. Laine,Gravitational wave background from Standard Model physics: Qualitative features,JCAP07(2015) 022 [1504."},{"citing_arxiv_id":"2604.15194","ref_index":42,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Dilaton-Flattened Axion Inflation","primary_cat":"hep-ph","submitted_at":"2026-04-16T16:24:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Dilaton backreaction on an anomaly-inspired axion potential generates a closed-form Lambert-W flattened hilltop, giving r ≈ 0.033–0.036 and α_s ≈ −4.6×10^{-4} at N=56 with strictly adiabatic dynamics.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"for the -trough benchmark branches. The quoted values follow from Eq. (49) evaluated on the benchmark trajectories and are independent of ¯wre. β N (0) ⋆ n(0) s r(0) 10 56.494 0.96863 0.03537 15 56.436 0.96860 0.03252 40 56.425 0.97110 0.03470 reheating boundary; values approaching 10 15 GeV are obtained in several otherwise consistent single-field and modified-gravity settings [42, 49, 50]. At the same time, explicit ultraviolet completions can narrow the viable win- dow: supersymmetric completions may be constrained by thermal or nonthermal gravitino production, while string-motivated embeddings can redistribute the inflaton energy into hidden sectors or moduli before the visible sec- tor thermalizes [37, 38, 51-58]. The temperatures quoted"},{"citing_arxiv_id":"2604.04764","ref_index":25,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational waves production during preheating within GB gravity with monomial coupling","primary_cat":"gr-qc","submitted_at":"2026-04-06T15:36:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"In Gauss-Bonnet inflation with monomial potential and coupling, gravitational waves from preheating produce a present-day energy density spectrum consistent with Planck constraints when the coupling strength, equation of state, and efficiency are set to specific values.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"This approach enables us to utilize the recent observational data provided by Planck experiments [24]. Furthermore, the preheating phase is characterized by the equation-of-state (EoS) parameter,ω, which describes the cosmic fluid and is defined asω=p/ρ. In our analysis, we assume that this EoS remains constant during this era, satisfying the following interval−1/3≤ω≤1. The lower bound ensures that the reheating expansion is not accelerated [25], while the upper bound is required to preserve causality. We also introduce an additional key parameter,δ, which represents the efficiency of the preheating process relating the energy density at the end of inflation,ρ end, to that at the end of preheating,ρ pre [42]. Moreover, the explosive production of particles during preheating produce large and significant inhomogeneity, which"},{"citing_arxiv_id":"2602.00317","ref_index":43,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reheating in geometric Weyl-invariant Einstein-Cartan gravity","primary_cat":"gr-qc","submitted_at":"2026-01-30T21:12:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Reheating temperature and equation-of-state parameter assumptions in Weyl-invariant Einstein-Cartan gravity models significantly alter predicted inflationary observables.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.13465","ref_index":19,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Equation of state during (p)reheating with trilinear interactions","primary_cat":"astro-ph.CO","submitted_at":"2025-07-17T18:16:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Lattice simulations show that the post-inflationary equation of state with trilinear interactions returns to zero after an initial deviation, substantially lowering stochastic gravitational wave amplitudes relative to prior estimates.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.10534","ref_index":83,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"ACT-ing on inflation: Implications of non Bunch-Davies initial condition and reheating on single-field slow roll models","primary_cat":"astro-ph.CO","submitted_at":"2025-05-15T17:45:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Non-Bunch-Davies initial conditions substantially improve the fit of various single-field slow-roll inflation models to updated n_s-r constraints from ACT DR6 combined with Planck, DESI, and BICEP/Keck data.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"when NBD corrections are taken into account. For n > 4, the situation is reversed: a lower reheating temperature provides a broader allowed parameter space in α to satisfy the desired nS while remaining consistent with the bound onrunder NBD corrections. B.ϕ n potential Let us now consider the scenarios of chaotic inflation with the potential having the monomial form as [ 83, 97, 98] V(ϕ) =V 0 \u0012 ϕ MPl \u0013n ,(31) where n is a positive constant. In our scenario, we shall consider the case of 0 .1 ≤n≤ 2. In such a model, it is very trivial to obtain the slow roll parameters, which have the following forms ϵ= n2M2 Pl 2ϕ2 , η= n(n−1)M 2 Pl ϕ2 .(32) And the number of e-folds during inflation is given by Nk = 1 2nM2 Pl (ϕ2 k −ϕ 2"},{"citing_arxiv_id":"2407.01713","ref_index":48,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Precision Inflationary Predictions: Impact of Accurate End-of-Inflation Dynamics","primary_cat":"astro-ph.CO","submitted_at":"2024-07-01T18:41:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Improved end-of-inflation dynamics shift the Starobinsky model's predicted spectral index n_s by up to 1.2×10^{-3} within the allowed reheating range.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.10295","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Einstein or Jordan: seeking answers from the reheating constraints","primary_cat":"gr-qc","submitted_at":"2019-07-24T08:27:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Differences in inflationary energy scales between Einstein and Jordan frames produce distinct reheating e-folding numbers and temperatures, leading to contrasting thermal histories with potential observational signatures.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.04402","ref_index":46,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Lectures on Reheating after Inflation","primary_cat":"astro-ph.CO","submitted_at":"2019-07-09T20:36:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"Lecture notes providing a generic introduction to reheating after inflation, covering its theoretical, phenomenological, and observational aspects.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Billiards in Inflation Preheating,\"Phys. Rev. Lett.103 (2009) 071301, arXiv:0903.3407 [astro-ph.CO]. [44] S. Antusch, F. Cefala, and S. Orani, \"Gravitational waves from oscillons after inflation,\" arXiv:1607.01314 [astro-ph.CO] . [45] J. B. Munoz and M. Kamionkowski, \"Equation-of-State Parameter for Reheating,\"Phys. Rev. D91 no. 4, (2015) 043521,arXiv:1412.0656 [astro-ph.CO] . [46] L. Dai, M. Kamionkowski, and J. Wang, \"Reheating constraints to inflationary models,\" Phys. Rev. Lett.113 (2014) 041302, arXiv:1404.6704 [astro-ph.CO] . [47] J. Martin, C. Ringeval, and V. Vennin, \"Observing Inflationary Reheating,\"Phys. Rev. Lett. 114 no. 8, (2015) 081303,arXiv:1410.7958 [astro-ph.CO] . [48] J. Martin, C. Ringeval, and V. Vennin, \"Information Gain on Reheating: the One Bit"}],"limit":50,"offset":0}