{"total":33,"items":[{"citing_arxiv_id":"2605.21092","ref_index":45,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Audible Axion Magnetogenesis: Linking Intergalactic Magnetic Fields and Gravitational Waves","primary_cat":"hep-ph","submitted_at":"2026-05-20T12:24:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Axion-like particles in the trapped misalignment mechanism produce observable gravitational waves while generating intergalactic magnetic fields that exceed blazar lower bounds in the parameter space promising for gravitational wave detection.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"01287 [astro-ph.CO]. [42] P. B. Greene, L. Kofman, A. D. Linde, and A. A. Starobinsky, Phys. Rev. D 56, 6175 (1997), arXiv:hep- ph/9705347. [43] L. Kofman, A. D. Linde, and A. A. Starobinsky, Phys. Rev. Lett. 73, 3195 (1994), arXiv:hep-th/9405187. [44] Y. Shtanov, J. H. Traschen, and R. H. Brandenberger, Phys. Rev. D 51, 5438 (1995), arXiv:hep-ph/9407247. [45] L. Kofman, A. D. Linde, and A. A. Starobinsky, Phys. Rev. D 56, 3258 (1997), arXiv:hep-ph/9704452. [46] J. F. Dufaux, A. Bergman, G. N. Felder, L. Kof- man, and J.-P. Uzan, Phys. Rev. D 76, 123517 (2007), arXiv:0707.0875 [astro-ph]. [47] A. Maleknejad, JHEP 07, 104 (2016), arXiv:1604.03327 [hep-ph]. [48] D. G. Figueroa and F. Torrenti, JCAP 02, 001 (2017),"},{"citing_arxiv_id":"2605.19825","ref_index":19,"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":"2605.09686","ref_index":46,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Asymmetric Reheating of Dark QED","primary_cat":"hep-ph","submitted_at":"2026-05-10T18:16:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Asymmetric reheating in Dark QED produces dark matter via a new channel where DM particles annihilate while still being created by inflaton decay, with the hidden-to-visible temperature ratio tied to the square root of the Yukawa coupling ratio.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.27103","ref_index":58,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Geodesically Complete Curvature-Bounce Inflation","primary_cat":"astro-ph.CO","submitted_at":"2026-04-29T18:47:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A closed k=+1 FRW universe with curvature-driven bounce and canonical scalar inflation remains sub-Planckian, satisfies the null energy condition, and produces ns=0.9617-0.9650 and r=0.0037-0.0045 consistent with data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.25635","ref_index":57,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Numerical Investigations of Stable Dynamics in the Presence of Ghosts","primary_cat":"math.DS","submitted_at":"2026-04-28T13:35:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Numerical simulations show ghost-normal scalar systems can remain dynamically bounded for long times when initial data is ultraviolet-dominated and low-amplitude, with some nonlinear potentials creating transient metastable states.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.21535","ref_index":7,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Fermion Condensate Inflation, Dynamical Waterfall Mechanism and Primordial Black Holes","primary_cat":"hep-th","submitted_at":"2026-04-23T10:59:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Torsion-induced fermion condensate produces hybrid inflation with axial-chemical-potential waterfall, Q-ball PBH seeds, and parity-violating signatures in Chern-Simons gravity.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"extended to nonthermal effects, such as parametric reso- nance, which can exponentially amplify inhomogeneities in the inflaton field. This stage is referred to as preheat- ing [4, 6]. Under certain conditions, these oscillations can become unstable due to nonlinear effects, causing the in- flaton to fragment into localized, non-topological solitons such as oscillons or Q-balls [7, 8]. The fragmentation of Q-balls provides an intriguing aspect in cosmology and astrophysics [9-16]. Q-balls are stable configurations of scalar fields that carry a con- served global charge and arise in theories with attrac- tive self-interactions. Their formation during inflation can significantly alter the post-inflationary evolution of the universe, as they can dominate the energy density"},{"citing_arxiv_id":"2604.20481","ref_index":12,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Dilaton-Induced Resonant Production of Ultralight Vector Dark Matter","primary_cat":"hep-ph","submitted_at":"2026-04-22T12:14:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Resonant dilatonic coupling produces ultralight vector dark matter with relic mass scaling as m_γ' ∝ r_i^{-2} for subdominant spectators in radiation-dominated backgrounds.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"spacetime written in conformal timeτ, with line element ds2 =a(τ) 2(dτ 2 −dx 2) and scale factora(τ). Through- out the regime of interest the spectator remains ener- getically subdominant until the Hubble rate drops to H≃m ϕ, so that its homogeneous evolution is well ap- proximated by overdamped freezing forH≫m ϕ and by coherent oscillations in the quadratic potential once H≲m ϕ [12, 13, 34, 35]. In Fourier space, with comoving wavevectorkand unit vector ˆk≡k/k, we decompose the spatial vector into two transverse polarizations and one longitudinal polar- 3 ization as Ai(τ,k) = X λ=± ϵ(λ) i (ˆk)Aλ(τ, k) + ˆkiAL(τ, k),(4) whereϵ (λ) i are transverse polarization vectors satisfying ˆk·ϵ (λ) = 0,A λ denotes the transverse mode functions,"},{"citing_arxiv_id":"2604.17478","ref_index":48,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A Unified Bogoliubov Approach to Primordial Gravitational Waves: From Inflation to Reheating","primary_cat":"hep-ph","submitted_at":"2026-04-19T15:09:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"An improved Bogoliubov numerical method computes the full primordial GW spectrum from inflation to reheating and shows that inflaton anharmonicity imprints distinctive features at high frequencies.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"For instance, despite the well-known resemblance between the Starobinsky model and a certain type of theα-attractor T model, the former can cause much more significant - 20 - wiggles on the spectrum than the latter. Such features could be important for probing inflationary models and the related reheating dynamics. Note added: As we were finalizing this work, we received a preprint from the authors of Ref. [48], which contains some overlap with this work. Ref. [48] mainly addresses the equiva- lence between the Bogoliubov and Boltzmann approaches in describing graviton production from the inflaton condensate. Our work is more focused on building a unified Bogoliubov approach that can be applied to the full-spectrum calculation. Hence there is substantial"},{"citing_arxiv_id":"2604.16085","ref_index":24,"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":"Brandenberger,Universe reheating after inflation, Phys. Rev. D51(1995) 5438 [hep-ph/9407247]. [22] L. Kofman, A.D. Linde and A.A. Starobinsky,Reheating after inflation,Phys. Rev. Lett.73 (1994) 3195 [hep-th/9405187]. [23] D. Boyanovsky, H.J. de Vega, R. Holman and J.F.J. Salgado,Analytic and numerical study of preheating dynamics,Phys. Rev. D54(1996) 7570 [hep-ph/9608205]. [24] L. Kofman, A.D. Linde and A.A. Starobinsky,Towards the theory of reheating after inflation,Phys. Rev. D56(1997) 3258 [hep-ph/9704452]. [25] A.A. Starobinsky,A New Type of Isotropic Cosmological Models Without Singularity,Phys. Lett. B91(1980) 99. [26] A.H. Guth,The Inflationary Universe: A Possible Solution to the Horizon and Flatness Problems,Phys."},{"citing_arxiv_id":"2604.15194","ref_index":45,"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":"JCAP2015(04), 047, arXiv:1502.04673 [astro-ph.CO]. [43] L. Kofman, A. Linde, and A. A. Starobinsky, Reheating af- ter inflation, Phys. Rev. Lett.73, 3195 (1994), arXiv:hep- th/9405187 [hep-th]. [44] L. Kofman, A. Linde, and A. A. Starobinsky, Towards the theory of reheating after inflation, Phys. Rev. D56, 3258 (1997), arXiv:hep-ph/9704452 [hep-ph]. [45] B. A. Bassett, S. Tsujikawa, and D. Wands, Inflation dynamics and reheating, Rev. Mod. Phys.78, 537 (2006), arXiv:astro-ph/0507632 [astro-ph]. [46] R. Allahverdi, R. Brandenberger, F.-Y. Cyr-Racine, and A. Mazumdar, Reheating in inflationary cosmology: The- ory and applications, Ann. Rev. Nucl. Part. Sci.60, 27 (2010), arXiv:1001.2600 [hep-th]. [47] M."},{"citing_arxiv_id":"2604.14480","ref_index":20,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Wave-envelope dark matter beyond the monochromatic paradigm","primary_cat":"hep-ph","submitted_at":"2026-04-15T23:32:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Mixing of ultralight wave dark matter fields creates a wave-envelope structure with intrinsic slow modulation and frequency sidebands, violating the standard monochromatic assumption.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"D108, 095028 (2023), arXiv:2305.16900 [hep-ph]. [17] P. Mart' ınez-Mirav' e, Y. F. Perez-Gonzalez, and M. Sen, Phys. Rev. D110, 055005 (2024), arXiv:2406.01682 [hep- ph]. [18] Y. Kim and H.-S. Lee, JHEP07, 269 (2025), arXiv:2503.04949 [hep-ph]. [19] L. Kofman, A. D. Linde, and A. A. Starobinsky, Phys. Rev. Lett.73, 3195 (1994), arXiv:hep-th/9405187. [20] L. Kofman, A. D. Linde, and A. A. Starobinsky, Phys. Rev. D56, 3258 (1997), arXiv:hep-ph/9704452. [21] P. B. Greene, L. Kofman, A. D. Linde, and A. A. Starobinsky, Phys. Rev. D56, 6175 (1997), arXiv:hep- ph/9705347. [22] P. B. Greene, L. Kofman, and A. A. Starobinsky, Nucl. Phys. B543, 423 (1999), arXiv:hep-ph/9808477. [23] J. Soda and Y. Urakawa, Eur."},{"citing_arxiv_id":"2604.12687","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Graviton Production from Inflaton Condensate: Boltzmann vs Bogoliubov","primary_cat":"hep-ph","submitted_at":"2026-04-14T12:58:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"For quadratic inflaton potentials Boltzmann and Bogoliubov spectra agree at short wavelengths, but for steeper potentials non-adiabatic transition effects captured only by Bogoliubov are sizable across a broad momentum range.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"of such initial state. The solution to Eq. (4.7) can be parametrized with the Bogoliubov coefficients [21] hk(τ) = αk(τ)p 2ωk(τ) e−i R τ ωk(τ ′)dτ ′ + βk(τ)p 2ωk(τ) e+i R τ ωk(τ ′)dτ ′ .(4.9) We note that the initial condition Eq. (4.8) corresponds toα k →1, andβ k →0. It follows from Eq. (4.9) that ωkhk −ih ′ k = r ωk 2 2βke+i R ωkdτ .(4.10) which leads to [13, 21] |βk|2 = 1 2ωk |ωkhk −ih ′ k|2 .(4.11) Using Eq. (4.9) and Eq. (4.7), one obtains the differential equations of the Bo- goliubov coefficients α′ k = ω′ k 2ωk e2i R τ ωk(τ ′)dτ ′ βk, β ′ k = ω′ k 2ωk e−2i R τ ωk(τ ′)dτ ′ αk.(4.12) After solving the background equations in Eq. (2.4), Eqs. (4.7) or (4.12) are solved numerically to obtain the number density."},{"citing_arxiv_id":"2604.09843","ref_index":68,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Induced Multi-phase Inflation with Reheating: Leptogenesis and Dark Matter Production in Metric versus Palatini","primary_cat":"hep-ph","submitted_at":"2026-04-10T19:17:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Multi-phase non-minimal inflation in metric and Palatini gravity predicts ns between 0.93 and 0.98, r up to 0.03 in metric but below 10^{-5} in Palatini, with non-thermal DM and leptogenesis viable for couplings in the 10^{-7} to 10^{-3} range.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"and in some cases may be impossible, depending on the functional form of the potential. In such situations, it is convenient to perform numerical computations of the inflationary dynamics directly in terms of the original scalar fieldϕ, without explicitly transforming to the canonical fieldζ. Accordingly, the slow-roll parameters must be expressed in terms of ϕ, and take the following form [68] ϵϕ = 1 2 \u0012 Vϕ V \u00132 , η ϕ = Vϕϕ V , κ 2 ϕ = VϕVϕϕϕ V 2 ,(16) where subscripts denote derivative with respect to the scalar fieldϕ. Then, the slow-roll parameters can be written as ϵ=Zϵ ϕ , η=Zη ϕ + sgn(V ′)Z ′ r ϵϕ 2 .(17) 9 Here,Z(ϕ) = (Π(ϕ)) −1 denotes the field-space metric, with Π(ϕ) defined in Eq. (5). The number ofe-folds between the horizon exit atϕ ∗ and the end of inflation atϕ e is then given"},{"citing_arxiv_id":"2604.07326","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Analytic Approximations for Fermionic Preheating","primary_cat":"hep-ph","submitted_at":"2026-04-08T17:42:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Analytic approximations for fermion number density in λφ⁴ preheating scale as q^{1/2} for q ≲ 0.01 and q^{3/4} for q ≳ 10, with resonance peaks or half-filled Fermi spheres depending on the coupling.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"nism of preheating is described by an oscillator-like differential equation (called the 'mode equation') and the number density per mode of the fermions produced is described by a model-independent equation. The method of calculating it involves techniques, such as Bo- goliubov transformations [8], that are well defined in the context of particle production from time-dependent background fields [9] and are also used in gravitational particle production [10] and the production of particles from an oscillating axion field [11, 12]. Particle production through preheating in the early universe affects the expansion history of the universe. It leads to different kinetic distributions and number densities of particles in the early universe than what is expected from perturbative reheating, which may lead to"},{"citing_arxiv_id":"2604.07256","ref_index":28,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Revisiting the sphaleron and axion production rates in QCD at high temperatures","primary_cat":"hep-lat","submitted_at":"2026-04-08T16:17:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Lattice QCD computations in thermal effective field theory yield sphaleron rates and axion production rates that deviate from perturbative estimates at high temperatures.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"tion of time (at sufficiently late times) for a non-thermal (top) SU(3) and (bottom) SU(2) plasma where the infrared glu- ons are over-occupied, shown for two different lattice with Qs.a= 1 (blue) andQ s.a= 0.5 (orange) respectively. production of particles is∼ g2 ΦΦ2 m2 Φ , wherem Φ is the mass of the inflaton. This ratio can be non-perturbatively large leading to efficient preheating of the universe [28]. A possible scenario extensively discussed in the literature involves inflaton coupling weakly to a thermal bath of radiation and decaying slowly through perturbative in- teractions [29-31]. Since the typical mass of the infla- ton is large it will decay into very high energy standard model particles, say for e.g., gluons. Based on Boltz- mann kinetic theory approach, the typical time-scale in"},{"citing_arxiv_id":"2604.05078","ref_index":35,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational Waves from Matter Perturbations of Spectator Scalar Fields","primary_cat":"hep-ph","submitted_at":"2026-04-06T18:29:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A spectator scalar field with strong portal coupling to the inflaton sources a stochastic gravitational wave background reaching Ω_GW h² ∼ 10^{-11} at frequencies 10^7-10^8 Hz for benchmark parameters σ/λ ≃ 10^4 and T_reh = 2×10^{14} GeV.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"preclude a spectrum that grows rapidly at shorter wavelengths. In particular, a blue-tilted spectator spectrum can become substantial on scalesk≫k ∗, beyond the reach of present CMB measurements, with potentially observable secondary signatures [30-34]. In our previous work [31-34], we showed that blue-tilted spectator spectra arise naturally when the effective mass satisfiesm χ,eff ≳0.5H ∗ [35], and that the resulting second-order GW background can strengthen this bound tom χ,eff ≳0.7H ∗. Those studies focused on spectators with small or vanishing portal couplings, for which gravitational particle production is the dominant production mechanism. The present work goes beyond this regime by considering large portal couplings, where parametric"},{"citing_arxiv_id":"2604.04764","ref_index":21,"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":"Errahmani and T. Ouali, \"Constraints on the reheating phase after Higgs inflation in the hybrid metric-Palatini approach,\" Phys. Lett. B853, 138679 (2024) [gr-qc/2404.15535]. [20] F. Bargach, A. Bargach, B. Asfour, A. Oukouiss and T. Ouali, \"Reheating constraints for an induced gravity model with a holographic description,\" Phys. Dark Univ.50, 102080 (2025). [21] L. Kofman, A. D. Linde and A. A. Starobinsky, \"Towards the theory of reheating after inflation,\" Phys. Rev. D56, 3258-3295 (1997) [hep-ph/9704452]. [22] P. B. Greene, L. Kofman, A. D. Linde and A. A. Starobinsky, \"Structure of resonance in preheating after inflation,\" Phys. Rev. D56, 6175-6192 (1997) [hep-ph/9705347]. [23] A. D. Dolgov and D. P. Kirilova, \"ON PARTICLE CREATION BY A TIME DEPENDENT SCALAR FIELD,\" Sov."},{"citing_arxiv_id":"2602.10215","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational scalar production with a generic reheating scenario","primary_cat":"hep-ph","submitted_at":"2026-02-10T19:06:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Gravitational scalar production yields reheating-dependent constraints on dark matter scalars, with dilution preserving viability for k<4 low-temperature reheating and factorization in multi-stage cases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2602.07972","ref_index":22,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Self-resonance preheating in deformed attractor models: oscillon formation and evolution","primary_cat":"astro-ph.CO","submitted_at":"2026-02-08T13:51:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Deformed alpha-attractor T-models with a Gaussian feature near the minimum yield more smaller shorter-lived oscillons during self-resonance preheating, suppressing energy in oscillons and altering the high-frequency gravitational wave tail while leaving low frequencies unchanged.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[18] M. Gleiser, Phys. Rev. D49, 2978 (1994), arXiv:hep- ph/9308279. [19] M. A. Amin, (2010), arXiv:1006.3075 [astro-ph.CO]. [20] M. A. Amin, R. Easther, and H. Finkel, JCAP12, 001, arXiv:1009.2505 [astro-ph.CO]. [21] M. A. Amin, R. Easther, H. Finkel, R. Flauger, and M. P. Hertzberg, Phys. Rev. Lett.108, 241302 (2012), arXiv:1106.3335 [astro-ph.CO]. [22] B. A. Bassett, S. Tsujikawa, and D. Wands, Rev. Mod. Phys.78, 537 (2006), arXiv:astro-ph/0507632 [astro- ph]. [23] R. Allahverdi, R. Brandenberger, F.-Y. Cyr-Racine, and A. Mazumdar, Ann. Rev. Nucl. Part. Sci.60, 27 (2010), arXiv:1001.2600 [hep-th]. [24] K. D. Lozanov, (2019), arXiv:1907.04402 [astro- ph.CO]. [25] M. A. Amin, M. P. Hertzberg, D. I."},{"citing_arxiv_id":"2602.06027","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"ACT DR6+Planck impact on inflation with non-zero vacuum expectation value and the post-inflationary behavior","primary_cat":"astro-ph.CO","submitted_at":"2026-02-05T18:57:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Updated constraints on non-zero VEV parameter M from ACT+Planck data, plus lattice simulations showing oscillon formation and reheating implications.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.00378","ref_index":36,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"High Frequency Spectrum of Primordial Gravitational Waves","primary_cat":"hep-ph","submitted_at":"2026-01-01T16:02:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"High-frequency primordial gravitational waves extend to higher frequencies due to post-inflation inflaton dynamics, and their detailed spectrum shape can distinguish inflation models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.17089","ref_index":160,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gauging Open EFTs from the top down","primary_cat":"hep-th","submitted_at":"2025-12-18T21:35:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Derives gauge-invariant influence functionals for photons and Stueckelberg fields in open U(1) gauge EFTs via BRST on the in-in contour after integrating out matter.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"that justify a gradient expansion are typically the same conditions that suppress environmental effects. In cosmology we expect open system effects become relevant whenever at least one of the follow- ing is present: (i) light (eg., gapless) degrees of freedom interact with the system generating memory effects and damping [159], (ii) strongly coupled or otherwise non-perturbative regimes (eg., reheat- ing/preheating [160], electroweak phase transitions [161]), (iii) horizons, (eg., cosmological/black-hole horizons [162-164]), iv) stochastic backreaction [165, 166]. 8 Conclusions In this work, we clarified the description of gauge theories for open systems and how it differs from the familiar case of open systems with global symmetries. We have emphasized the power of the BRST"},{"citing_arxiv_id":"2512.07284","ref_index":42,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Evaporation of Primordial Black Holes in a Thermal Universe: A Thermofield Dynamics Approach","primary_cat":"hep-th","submitted_at":"2025-12-08T08:22:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Thermal bath corrections derived via thermofield dynamics enhance the evaporation rate of primordial black holes, shortening their lifetimes relative to zero-temperature calculations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.00152","ref_index":113,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Every Wrinkle Carries A Memory: An Integro-differential Bootstrap for Features in Cosmological Correlators","primary_cat":"hep-th","submitted_at":"2025-10-31T18:00:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"Derives integro-differential boundary equations from bulk locality for scale-breaking cosmological correlators with oscillating heavy-field masses and solves them analytically and numerically to reveal enhanced collider signals.","context_count":1,"top_context_role":"background","top_context_polarity":"support","context_text":"hypergeometric function of higher weight (4.53),F(k, k) still retains one layer of summation 28. Then, after applying the relevant relation (4.81), we can finally estimate the power spectrum as O(g2) : ∆P(k) P(k) ∼ O(0.1)×r 1 g2 ,(4.94) these features are tightly constrained by CMB experiments, with their amplitude required to be less than a few percent [113]. This constraint translates into the boundr 1g2 <10 −1. The bispectrum amplitude, nevertheless, is determined by the parameterr 2 rather thanr 1, with the two related throughr 2 = (∆−1 ζ H/Λ √ 2π) √r1. Thanks to the enhancement factor ∆ −1 ζ ∼10 4, the resulting bispectrum can still be appreciably large despite the tight constraint on the features of"},{"citing_arxiv_id":"2510.25505","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Resonant production of millicharged scalars in $k^2>0$ electromagnetic wave background","primary_cat":"hep-ph","submitted_at":"2025-10-29T13:30:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Resonant exponential growth of millicharged scalars in k²>0 electromagnetic waves is obtained by mapping the Klein-Gordon equation to the Mathieu equation, yielding new constraints on such particles.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.25013","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational waves from axion inflation in the gradient expansion formalism. Part II. Fermionic axion inflation","primary_cat":"astro-ph.CO","submitted_at":"2025-09-29T16:38:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Schwinger fermion production in axion inflation damps gauge fields, enabling observable primordial gravitational waves in LISA/ET bands while satisfying ΔN_eff limits and identifying a new damped-oscillation backreaction regime.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.13465","ref_index":32,"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":"2411.08691","ref_index":74,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Chiral Gravitational Wave Background from Audible Axion via Nieh-Yan Term","primary_cat":"hep-ph","submitted_at":"2024-11-13T15:26:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Axion-like fields coupled to the Nieh-Yan term generate a chiral GW background during radiation domination, with parameter space explored for detectability in PTA and space-based observatories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2407.01713","ref_index":42,"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":"2406.13394","ref_index":78,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational Wave Birefringence from Fuzzy Dark Matter","primary_cat":"gr-qc","submitted_at":"2024-06-19T09:38:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Fuzzy dark matter induces frequency-dependent amplitude birefringence in gravitational waves with periodic time modulation set by the scalar mass, but no velocity birefringence.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1912.02622","ref_index":217,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Science Case for the Einstein Telescope","primary_cat":"astro-ph.CO","submitted_at":"2019-12-05T14:57:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"The Einstein Telescope will enable gravitational-wave observations up to cosmological distances, opening avenues for discoveries in astrophysics, cosmology, and fundamental physics.","context_count":1,"top_context_role":"background","top_context_polarity":"support","context_text":"Lett. 73 (1994) 3195-3198, arXiv:hep-th/9405187 [hep-th] . [215] L. Kofman, A. D. Linde, and A. A. Starobinsky, \"Towards the theory of reheating after inflation,\" Phys. Rev. D56 (1997) 3258-3295, arXiv:hep-ph/9704452 [hep-ph] . [216] P. B. Greene and L. Kofman, \"Preheating of fermions,\" Phys. Lett. B448 (1999) 6-12, arXiv:hep-ph/9807339 [hep-ph] . [217] P. B. Greene and L. Kofman, \"On the theory of fermionic preheating,\" Phys. Rev. D62 (2000) 123516, arXiv:hep-ph/0003018 [hep-ph] . [218] D. G. Figueroa and E. H. Tanin, \"Ability of LIGO and LISA to probe the equation of state of the early Universe,\" JCAP 1908 (2019) 011, arXiv:1905.11960 [astro-ph.CO] . [219] N. Bartolo, D. Bertacca, S. Matarrese, M."},{"citing_arxiv_id":"1907.04402","ref_index":14,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1906.09299","ref_index":77,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Noncanonical Approaches To Inflation","primary_cat":"gr-qc","submitted_at":"2019-06-21T19:25:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"A review thesis covering Mukhanov parametrization, general scalar-tensor theories, and new slow-roll techniques for canonical and noncanonical inflation observables.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"depends on how the inflaton couples to the Standard Model particles. One important feature is that reheating occurs at t ∼ H−1 ∼ Γ−1, i.e. the reheating temperature is given byTreh∼√MPlΓ. As we shall discuss, an important and surprising feature of inflation is thattheprimordialperturbationsfreezeafterinflationhasfinished, i.e.their subsequentevolutionisnotaffectedbythephysicsofreheating(seeRefs.[15, 17,77-79] for more details on the reheating processes in the early universe). 2.2.4 Duration of inflation As the expansion is exponentially accelerated, the duration of inflation is parametrized by means of the number ofefolds ∆N ≡ ln (aend/ainitial). Therefore, the number ofefolds elapsed from a particular epoch to the end of inflation is given by N =  tend"}],"limit":50,"offset":0}