{"total":18,"items":[{"citing_arxiv_id":"2606.31975","ref_index":15,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Reheating in No-Scale Models of Inflation","primary_cat":"hep-ph","submitted_at":"2026-06-30T17:16:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Generalized no-scale models with R=2/(3α) for α≠1 or non-minimal gauge couplings allow unsuppressed inflaton decays, producing calculable reheating temperatures and (n_s,r) predictions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27521","ref_index":15,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"From WIMP to FIMP during reheating: collider vs non-collider probes for p-wave annihilation","primary_cat":"hep-ph","submitted_at":"2026-05-26T18:00:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Collider experiments can strongly constrain p-wave-suppressed derivative operators and thereby limit reheating temperature, DM mass, and interaction scale needed to match observed DM abundance during reheating.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"At the end of the reheating (a=a rh), the energy densities of the inflaton and radiation are equal,ρ R(arh) =ρ ϕ(arh) = 3M 2 P H(arh)2. Note that, to avoid affecting the success of BBN, the reheating temperatureT rh must satisfyT rh > T BBN ≃4 MeV [59-64]. The evolution of the SM radiation energy densityρ R, on the other hand, is governed by the Boltzmann equation of the form [15] dρR dt + 4Hρ R = + 2n 2 +n Γϕ ρϕ .(3.8) Using Eq. (3.6), one can solve Eq. (3.8) and further obtain ρR(a)≃ 2 √ 3n 2 +n MP a4 Z a aI Γϕ(a′) q ρϕ(a′)a ′3 da′ .(3.9) Note that here a general scale factor dependence of Γ ϕ has been assumed, which may arise, for example, from the field-dependent inflaton mass. In the present setup, the effective mass mϕ(a) for the inflaton can be obtained from the second derivative of Eq."},{"citing_arxiv_id":"2605.24163","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Leptogenesis without on-shell right-handed neutrinos","primary_cat":"hep-ph","submitted_at":"2026-05-22T19:33:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"A four-body decay of a new scalar via off-shell right-handed neutrinos generates sufficient CP asymmetry to explain the observed baryon asymmetry in two cosmological scenarios.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19825","ref_index":25,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2605.05310","ref_index":51,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constraints on the inflationary vacuum and reheating era from NANOGrav","primary_cat":"astro-ph.CO","submitted_at":"2026-05-06T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"NANOGrav data favors a blue-tilted tensor spectrum with nt ≈ 2.2, radiation-dominated reheating, and alpha-vacuum states over standard Bunch-Davies, with a frequency-dependent alpha suggested to resolve the blue-tilt tension.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Bardeen,Gauge-invariant cosmological perturbations,Phys. Rev. D22(1980) 1882. [48] H. Kodama and M. Sasaki,Cosmological Perturbation Theory,Prog. Theor. Phys. Suppl.78 (1984) 1. [49] K.A. Malik and D. Wands,Cosmological perturbations,Phys. Rept.475(2009) 1 [0809.4944]. [50] C. Caprini and D.G. Figueroa,Cosmological backgrounds of gravitational waves,Class. Quant. Grav.35(2018) 163001 [1801.04268]. [51] N. Christensen,Stochastic Gravitational Wave Backgrounds,Rept. Prog. Phys.82(2019) 016903 [1811.08797]. - 17 - [52] A.R. Liddle and D.H. Lyth,The Cold dark matter density perturbation,Phys. Rept.231 (1993) 1 [astro-ph/9303019]. [53]Planckcollaboration,Planck 2018 results. VI. Cosmological parameters,Astron. Astrophys. 641(2020) A6 [1807.06209]. [54] E."},{"citing_arxiv_id":"2605.03014","ref_index":62,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Searching for UFOs from the early universe: direct detection prospects for relativistically decoupling dark matter","primary_cat":"hep-ph","submitted_at":"2026-05-04T18:00:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Ultrarelativistically decoupling dark matter in Z' portal models has direct detection cross sections that existing experiments like LZ and XENONnT have already excluded over large regions, leaving testable space above the neutrino fog for 0.4 GeV to 1 TeV masses.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Turner, Phys. Rev. D31, 681 (1985) [60] G. F. Giudice, E. W. Kolb and A. Riotto, Phys. Rev. D64(2001) 023508 [hep-ph/0005123]; D. J. H. Chung, E. W. Kolb and A. Riotto, Phys. Rev. D60(1999) 063504 [hep-ph/9809453]. - 27 - [61] M. A. G. Garcia, K. Kaneta, Y. Mambrini and K. A. Olive, Phys. Rev. D101(2020) no.12, 123507 [arXiv:2004.08404 [hep-ph]. [62] M. A. G. Garcia, K. Kaneta, Y. Mambrini and K. A. Olive, JCAP04, 012 (2021) [arXiv:2012.10756 [hep-ph]]. [63] C. A. J. O'Hare, Phys. Rev. Lett.127, no.25, 251802 (2021) [arXiv:2109.03116 [hep-ph]]. [64] Y. Mambrini, Particles in the dark Universe,Springer Ed., ISBN 978-3-030-78139-2 (2021). [65] M. Srednicki, R. Watkins and K. A. Olive, Nucl. Phys."},{"citing_arxiv_id":"2604.16085","ref_index":71,"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":"11The application of the perturbative approach from [133, 138] beyond regime (i) to study DM production is conceptually questionable and introduces an error the size of which cannot be quantified within this scheme. The range of validity of perturbative methods can be extended by the introduction of effective time dependent masses and decay rates [71] in the averaged equations of motion (2.6), though the results found in [55] indicate that this approach can already fail within regime (ii), implying that the results obtained for several DM candidates may need revision, cf. Sec. 5. 12While the authors of [32] have chosen values forgthat are small enough to justify a perturbative treatment, the part of their study using potentialsV(ϕ)∝ϕ j withj >2violates condition (2."},{"citing_arxiv_id":"2604.14620","ref_index":24,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Inflaton Regeneration via Scalar Couplings: Generic Models and the Higgs Portal","primary_cat":"hep-ph","submitted_at":"2026-04-16T05:02:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"For monomial inflationary potentials with k≥4, the inflaton regenerates from the thermal bath after reheating because its amplitude-dependent mass vanishes asymptotically.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"3755 [hep-th]. [21] R. Kallosh, A. Linde, and D. Roest, \"Superconformal Inflationaryα-Attractors,\"JHEP11 (2013) 198,arXiv:1311.0472 [hep-th]. [22] R. Kallosh and A. Linde, \"Universality Class in Conformal Inflation,\"JCAP07(2013) 002, arXiv:1306.5220 [hep-th]. [23] D. Roest, \"Universality classes of inflation,\"JCAP01(2014) 007,arXiv:1309.1285 [hep-th]. [24] R. Kallosh, A. Linde, and D. Roest, \"Large field inflation and doubleα-attractors,\"JHEP 08(2014) 052,arXiv:1405.3646 [hep-th]. [25] M. S. Turner, \"Coherent Scalar Field Oscillations in an Expanding Universe,\"Phys. Rev. D 28(1983) 1243. [26] M. A. G. Garcia, K. Kaneta, Y. Mambrini, and K. A. Olive, \"Inflaton Oscillations and Post-Inflationary Reheating,\"JCAP04(2021) 012,arXiv:2012."},{"citing_arxiv_id":"2604.12687","ref_index":42,"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":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"8 n s n(n+ 2) |n−4| X j>0 |Vj| j3/2 \u0012 He ˜me \u00133/2\u0012 as ae \u0013− 9 n+2 , ≃ 3√π 8 n s n(n+ 2) |n−4| X j>0 |Vj| j3/2 \u0012 He ˜me \u00133/2\u0012 nk 2j˜meae \u0013 9 2(n−4) .(4.25) - 14 - We have usedρ ϕ ∝H 2 ∝a −3(1+ω) at second and third equalities, where a decay factor is omitted forρ ϕ, because for generaln, the decay cannot be described in terms of simple exponential [42]. Eq. (4.23) is used at second and fourth equalities and ˜m= ˜me(a/ae)−3ω is used at third equality. In the last step, the solution to Eq. (4.23) is inserted. We notice that just like in the Boltzmann case, the spectrum diverges withn= 4. There are similarities and differences between the Boltzmann method and sta- tionary phase approximation within the Bogoliubov framework."},{"citing_arxiv_id":"2604.09356","ref_index":94,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"CMB signatures of gravity-mediated dark radiation in $\\mathbf{\\Delta N_{\\rm eff}}$","primary_cat":"hep-ph","submitted_at":"2026-04-10T14:29:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Gravity-mediated production of scalar and vector dark radiation yields Planck 2018 constraints on reheating temperature T_RH and background equation of state w_Φ, with comparisons to right-handed neutrinos, ALPs, and a generic spin-2 mediator.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Ghoshal, A. Naskar and N. Okada,Unified origin of curvature perturbation and baryon asymmetry of the universe,JHEP01(2026) 082, [2410.07694]. [92] B. D. Fields, K. A. Olive, T.-H. Yeh and C. Young,Big-Bang Nucleosynthesis after Planck, JCAP03(2020) 010, [1912.01132]. [93]CMB-HDcollaboration, S. Aiola et al.,Snowmass2021 CMB-HD White Paper,2203.05728. [94]Simons Observatorycollaboration, P. Ade et al.,The Simons Observatory: Science goals and forecasts,JCAP02(2019) 056, [1808.07445]. - 26 - [95] S. Ghosh, S. Kumar and Y. Tsai,Free-streaming and coupled dark radiation isocurvature perturbations: constraints and application to the Hubble tension,JCAP05(2022) 014, [2107.09076]. [96] X. Luo, W. Rodejohann and X."},{"citing_arxiv_id":"2604.05078","ref_index":67,"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":"The end of inflation is defined byε≡ − ˙H/H 2 = 1, or equivalentlyd(1/aH)/dη= 0, when the comoving Hubble radius reaches its minimum. For a canonical single field, the Friedmann equations imply ˙ϕ2 =V(ϕ) atε= 1, giving ρend ≡ρ ϕ(aend) = 3 2 V(ϕ end), H 2 end = V(ϕ end) 2M 2 P .(2.8) Current CMB data tightly constrain the inflationary parameter space. BICEP/Keckreportsr < 0.036 (95% C.L.) [67] while combined analyses yield the scalar spectral tiltn s ≃0.965± O(10 −3) [29, 68]. These benchmarks favor plateau-like potentials, including Starobinsky inflation [69, 70] andα- attractor models such as the T-model [71, 72]. For concreteness in our explicit calculations we adopt the quadratic T-model potential V(ϕ) =λM 4 P \u0014√ 6 tanh \u0012 ϕ√ 6M P \u0013\u00152"},{"citing_arxiv_id":"2602.10215","ref_index":21,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":136,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"unclear","context_text":"[133] J. F. Dufaux, A. Bergman, G. N. Felder, L. Kof- man, and J.-P. Uzan, Phys. Rev. D76, 123517 (2007), arXiv:0707.0875 [astro-ph]. [134] F. Li, N. Yang, Z. Fang, R. M. L. Baker, Jr., G. V. Stephenson, and H. Wen, Phys. Rev. D80, 064013 (2009), arXiv:0909.4118 [gr-qc]. [135] T. Akutsuet al., Phys. Rev. Lett.101, 101101 (2008), arXiv:0803.4094 [gr-qc]. [136] A. S. Chouet al.(Holometer), Phys. Rev. D95, 063002 (2017), arXiv:1611.05560 [astro-ph.IM]. [137] A. Patraet al., Phys. Rev. Lett.135, 101402 (2025), arXiv:2410.09175 [gr-qc]. [138] L. Pagano, L. Salvati, and A. Melchiorri, Phys. Lett. B 760, 823 (2016), arXiv:1508.02393 [astro-ph.CO]. [139] C. Caprini and D. G. Figueroa, Class. Quant. Grav.35, 163001 (2018), arXiv:1801."},{"citing_arxiv_id":"2601.20939","ref_index":32,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing Bose-enhanced Inflaton Decay with Gravitational Waves","primary_cat":"hep-ph","submitted_at":"2026-01-28T19:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bose enhancement from a transient condensate of inflaton decay products dramatically increases decay efficiency and amplifies stochastic gravitational wave production to potentially observable levels.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.07284","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2511.04933","ref_index":81,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Low-reheating scenario in dark Higgs inflation and its impact on dark photon dark matter production","primary_cat":"hep-ph","submitted_at":"2025-11-07T02:25:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A dark U(1)_D model with dark Higgs inflation and low reheating allows dark photon dark matter to achieve the observed relic density for a wider range of couplings, with inflation predictions matching Planck, BICEP/Keck and ACT data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.05967","ref_index":78,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Stochastic Gravitational Waves from Modulated Reheating","primary_cat":"astro-ph.CO","submitted_at":"2025-10-07T14:23:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A spectator scalar in modulated reheating with large Higgs-like couplings generates detectable scalar-induced stochastic gravitational waves for BBO and DECIGO, but only outside perturbative low-energy extrapolations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.10534","ref_index":78,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"B596, 306 (2004), arXiv:hep- th/0402038. [75] B. R. Greene, K. Schalm, G. Shiu, and J. P. van der Schaar, JCAP02, 001 (2005), arXiv:hep-th/0411217. [76] A. Ashoorioon, R. Casadio, G. Geshnizjani, and H. J. Kim, JCAP09, 008 (2017), arXiv:1702.06101 [hep-th]. [77] M. A. G. Garcia, K. Kaneta, Y. Mambrini, and K. A. Olive, JCAP04, 012 (2021), arXiv:2012.10756 [hep-ph]. [78] S. Clery, Y. Mambrini, K. A. Olive, and S. Verner, Phys. Rev. D105, 075005 (2022), arXiv:2112.15214 [hep-ph]. [79] S. Clery, Y. Mambrini, K. A. Olive, A. Shkerin, and S. Verner, Phys. Rev. D105, 095042 (2022), arXiv:2203.02004 [hep-ph]. [80] M. R. Haque and D. Maity, Phys. Rev. D107, 043531 (2023), arXiv:2201.02348 [hep-ph]. [81] M. Riajul Haque, E."}],"limit":50,"offset":0}