{"total":11,"items":[{"citing_arxiv_id":"2604.25635","ref_index":58,"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":"2604.20481","ref_index":36,"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":"[33] N. Kitajima, S. Nakagawa, F. Takahashi, and W. Yin, Phys. Lett. B857, 139304 (2025), arXiv:2410.17964 [hep- ph]. [34] R. Allahverdi, R. Brandenberger, F.-Y. Cyr-Racine, and A. Mazumdar, Ann. Rev. Nucl. Part. Sci.60, 27 (2010), arXiv:1001.2600 [hep-th]. [35] K. D. Lozanov and M. A. Amin, Phys. Rev. D97, 023533 (2018), arXiv:1710.06851 [astro-ph.CO]. [36] P. B. Greene, L. Kofman, A. Linde, and A. A. Starobin- sky, Phys. Rev. D56, 6175 (1997), arXiv:hep-ph/9705347 [hep-ph]."},{"citing_arxiv_id":"2604.07044","ref_index":37,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Post-Inflationary Quenched Production of Axion SU(2) Dark Matter","primary_cat":"hep-ph","submitted_at":"2026-04-08T12:59:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Post-inflationary axion-SU(2) vector dark matter production is recast as a quantum quench with a survival factor that induces an O(1) renormalization of the standard relic abundance.","context_count":1,"top_context_role":"extension","top_context_polarity":"extend","context_text":"through spontaneous symmetry breaking, the homoge- neous gauge amplitude obeys ¨Q+ 3H ˙Q+ \u0010 ˙H+ 2H 2 +m(t) 2 \u0011 Q+ 2g 2Q3 = 0,(3) where g is the SU(2) gauge coupling and H = ˙a/ais the Hubble parameter. In the unbroken phasem(t) = 0, this is a quartic oscillator dressed by expansion. In the broken phase the dynamics cross over to those of a massive vector. The inherited-condensate mechanism of [37] analyzes this transition adiabatically and infers the final abundance from the preserved invariant. Our aim is to retain the same homogeneous starting point while treating the transition itself as a dynamical quench. 3 B. Effective homogeneous Lagrangian A compact effective Lagrangian reproducing (3) is Leff = 3 2 a3 h ( ˙Q+HQ) 2 −g 2Q4 −m(t) 2Q2"},{"citing_arxiv_id":"2604.05078","ref_index":38,"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":", \"Milky Way Satellite Census. III. Constraints on Dark Matter Properties from Observations of Milky Way Satellite Galaxies,\"Phys. Rev. Lett.126(2021) 091101,arXiv:2008.00022 [astro-ph.CO]. [37] K. K. Boddyet al., \"Snowmass2021 theory frontier white paper: Astrophysical and cosmological probes of dark matter,\"JHEAp35(2022) 112-138,arXiv:2203.06380 [hep-ph]. [38] K. Kohri and T. Terada, \"Semianalytic calculation of gravitational wave spectrum nonlinearly induced from primordial curvature perturbations,\"Phys. Rev. D97no. 12, (2018) 123532, arXiv:1804.08577 [gr-qc]. [39] L. Kofman, A. D. Linde, and A. A. Starobinsky, \"Reheating after inflation,\"Phys. Rev. Lett.73 (1994) 3195-3198,arXiv:hep-th/9405187. [40] Y."},{"citing_arxiv_id":"2604.04764","ref_index":22,"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":"However, this mechanism can be slow and inefficient. Consequently, a preheating stage is incorporated as the onset of the reheating period. Preheating is an explosive, non-perturbative process that occurs immediately after inflation, during which the energy density of the inflaton is rapidly transferred to coupled fields through parametric resonance, producing a large number of particles [22, 23]. To constrain this post-inflationary epoch, it is necessary to relate its parameters, specifically the preheating duration, to those of reheating and inflation, such as the reheating duration, thermalization temperature, and spectral index. This approach enables us to utilize the recent observational data provided by Planck experiments [24]. Furthermore,"},{"citing_arxiv_id":"2602.10215","ref_index":16,"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":"2512.07284","ref_index":49,"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":"2511.02184","ref_index":38,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark Matter Freeze-in from a $Z^\\prime$ Reheaton","primary_cat":"hep-ph","submitted_at":"2025-11-04T01:57:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Dark matter freezes in from non-thermal Z' decays before reheating ends in an inflationary model with a secluded U(1)_D gauge sector, Z' reheaton, and lattice treatment of non-perturbative effects, opening viable parameter space with GW probes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.00152","ref_index":114,"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":"unclear","context_text":"Westphal,Gravity Waves and Linear Inflation from Axion Monodromy,Phys. Rev. D82(2010) 046003 [0808.0706]. [111] Z. Qin, T. Colas and X. Tong,To appear, . [112] A. Hook and R. Rattazzi,Softening the UV without new particles,Phys. Rev. D108 (2023) 115019 [2306.12489]. [113]Planckcollaboration,Planck 2018 results. X. Constraints on inflation,Astron. Astrophys.641(2020) A10 [1807.06211]. [114] L. Kofman, A.D. Linde and A.A. Starobinsky,Reheating after inflation,Phys. Rev. Lett. 73(1994) 3195 [hep-th/9405187]. [115] L. Kofman, A.D. Linde and A.A. Starobinsky,Towards the theory of reheating after inflation,Phys. Rev. D56(1997) 3258 [hep-ph/9704452]. [116] P.B. Greene, L. Kofman, A.D. Linde and A.A. Starobinsky,Structure of resonance in preheating after inflation,Phys."},{"citing_arxiv_id":"2507.13465","ref_index":33,"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":"1907.04402","ref_index":89,"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":"we briefly discuss their effects on various aspects of the non-perturbative linear dynamics - 51 - Figure 7. The instability chart featuring the real part of the Floquet exponent normalized by the effective inflaton mass (left) and the Hubble rate (right), characterizing theχ particle production rate in the Vanilla model of preheating,V (φ, χ) = λφ4/4+ g2φ2χ2, g2 > 0 [89]. In FRW space-time ¯Φ∝ a−1 and k∝ a−1, implying that co-moving modes do not flow across the chart as the universe expands unlike in Figs. 3, 4, 5. The resonance is virtually unaffected by the expansion of space. of preheating by considering simple toy models. We also talk about some generic models of (p)reheating. 7.1 Scalar fields Historically, non-perturbative effects during preheating were first studied in the context"}],"limit":50,"offset":0}