{"total":23,"items":[{"citing_arxiv_id":"2605.15197","ref_index":38,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Primordial Black Hole from Tensor-induced Density Fluctuation: First-order Phase Transitions and Domain Walls","primary_cat":"astro-ph.CO","submitted_at":"2026-05-14T17:59:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Tensor perturbations from first-order phase transitions and domain wall annihilation induce curvature fluctuations at second order that form primordial black holes, allowing asteroid-mass PBHs to comprise all dark matter for specific parameter ranges with associated gravitational wave peaks in LISA,","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"neither in terms of cosmic-ray fluxes [178, 182, 184-186], nor in terms of modification of the ionization fraction in CMB [212-214], nor in terms of modification of the abundance of light elements produced during BBN [186], we can exclude theorangeregions on the right side respectively labeled as \"Evaporation\". Finally, in dashed and solidgray we indicate where gravitational waves from bubble collision fall within the detectability of pulsar timing arrays [38, 40- 42, 215-219] and exclusion of LIGO-Virgo [220]. Additionally, in the region labeled \"BBN\" in brown, the reheating temperature is lower than the temperature of neutrino decoupling,T ⋆ ≲MeV [221], which is excluded. We present the allowed values forβ/Hforα≫1, 1, and 10 −1 in solid, dotted, and dashed respectively. The benchmark points shown in Table I are also depicted in Fig."},{"citing_arxiv_id":"2605.11332","ref_index":2,"ref_count":2,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Reviving primordial black hole formation in slow first-order phase transitions","primary_cat":"hep-ph","submitted_at":"2026-05-11T23:34:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Slow reheating after a supercooled first-order phase transition allows an early matter-dominated era in which small curvature perturbations grow sufficiently to form primordial black holes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"supported by startup funds from the Tsung-Dao Lee Institute and Shanghai Jiao Tong University. KPX is supported by the National Natural Science Foundation of China under Grant No. 12305108. [1] A. Mazumdar and G. White, \"Review of cosmic phase transitions: their significance and experimental signatures,\" Rept. Prog. Phys.82(2019) no. 7, 076901, arXiv:1811.01948 [hep-ph]. [2] C. Caprini et al., \"Detecting gravitational waves from cosmological phase transitions with LISA: an update,\"JCAP 03(2020) 024,arXiv:1910.13125 [astro-ph.CO]. [3] P. Athron, C. Balázs, A. Fowlie, L. Morris, and L. Wu, \"Cosmological phase transitions: From perturbative particle physics to gravitational waves,\"Prog. Part. Nucl. Phys.135 (2024) 104094,arXiv:2305."},{"citing_arxiv_id":"2605.03758","ref_index":71,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Dark Matter Production from Bubble Collisions during a First-Order Phase Transition at the End of Inflation","primary_cat":"hep-ph","submitted_at":"2026-05-05T13:42:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bubble collisions during a first-order phase transition at the end of inflation can generate the observed dark matter abundance in a restricted region of parameter space via direct production and spectator decays.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Sazhin and A.V. Veryaskin,Graviton Creation in the Inflationary Universe and the Grand Unification Scale,Phys. Lett. B115(1982) 189. [69] L.F. Abbott and M.B. Wise,Constraints on Generalized Inflationary Cosmologies,Nucl. Phys. 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Caprini et al.,Detecting gravitational waves from cosmological phase transitions with LISA: an update,JCAP03(2020) 024 [1910."},{"citing_arxiv_id":"2605.04110","ref_index":15,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"High-Power AM-CW Lunar Laser Ranging as a $\\mu$Hz SGWB Detector","primary_cat":"gr-qc","submitted_at":"2026-05-04T23:05:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"AM-CW lunar laser ranging achieves μHz SGWB sensitivity of 5.29×10^{-9} D_cov (80 μm range uncertainty) or 2.07×10^{-9} D_cov (50 μm) over 5 years, with discovery possible if covariance degradation stays below ~3.6-13.7.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.27376","ref_index":82,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Electroweak Baryogenesis from Collapsing Domain Walls","primary_cat":"hep-ph","submitted_at":"2026-04-30T03:40:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Collapsing axion-like domain walls generate the baryon asymmetry by acting as an effective chemical potential through coupling to the electroweak topological term, with the asymmetry produced via sphaleron processes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Lett.112, 041301 (2014), arXiv:1304.2433 [hep-ph]. [80] M. Hindmarsh, S. J. Huber, K. Rummukainen, and D. J. Weir, Phys. Rev. D92, 123009 (2015), arXiv:1504.03291 [astro-ph.CO]. [81] M. Hindmarsh, S. J. Huber, K. Rummukainen, and D. J. Weir, Phys. Rev. D96, 103520 (2017), [Erra- tum: Phys.Rev.D 101, 089902 (2020)], arXiv:1704.05871 [astro-ph.CO]. [82] C. Capriniet al., JCAP03, 024 (2020), arXiv:1910.13125 [astro-ph.CO]. [83] M. Vanvlasselaer and W. Yin, (2026), arXiv:2604.20762 [hep-ph]. [84] P. W. Graham, D. E. Kaplan, and S. Rajendran, Phys. Rev. Lett.115, 221801 (2015), arXiv:1504.07551 [hep- ph]. [85] J. R. Espinosa, C. Grojean, G. Panico, A. Pomarol, O. Pujol` as, and G. Servant, Phys. Rev."},{"citing_arxiv_id":"2604.25726","ref_index":106,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Imprint of domain wall annihilation on induced gravitational waves","primary_cat":"hep-ph","submitted_at":"2026-04-28T14:53:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Domain wall annihilation imprints a two-peaked spectrum on induced gravitational waves via an early matter-dominated phase and entropy dilution.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"using the broken power-law parametrization introduced 6 in Refs.[2, 105]: ΩGWh2 = Ωph2 D4/3 (a+b) c \u0012 b \u0010 D1/3 f fp \u0011−a/c +a \u0010 D1/3 f fp \u0011b/c\u0013c ,(36) wherea,bandcare real and positive parameters. Here the low-frequency slope4 a= 3can be fixed by causality, while numerical simulations suggestb≃c≃1[96]. InFig. 3, wefirstpresentthepower-lawintegratedsen- sitivity curves [106] of the future GW detectors ET [107], LISA [108], DECIGO [109],µAres [110], SKA [111], and THEIA [112] which are evaluated following Eq. (36) by calculating the signal-to-noise ratio (SNR) [113, 114] ϱ= \" ndettobs Z fmax fmin d f \u0012Ωsignal (f) Ωnoise (f) \u00132#1/2 , wheren det = 1for auto-correlated detectors andndet = 2 for cross-correlated detectors,t obs denotes the observa-"},{"citing_arxiv_id":"2604.21972","ref_index":7,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Matchotter: An Automated Tool for Dimensional Reduction at Finite Temperature","primary_cat":"hep-ph","submitted_at":"2026-04-23T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Matchotter automates one-loop finite-temperature dimensional reduction and supersoft matching for generic Lagrangians using functional techniques.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"A35(2020) 2050075, [1807.09495]. [5]LISA Cosmology Working Groupcollaboration, P. Auclair et al.,Cosmology with the Laser Interferometer Space Antenna,Living Rev. Rel.26(2023) 5, [2204.05434]. [6] K. Kajantie, M. Laine, K. Rummukainen and M. E. Shaposhnikov,Is there a hot electroweak phase transition atm H ≳m W ?,Phys. Rev. Lett.77(1996) 2887-2890, [hep-ph/9605288]. [7] F. Csikor, Z. Fodor and J. Heitger,Endpoint of the hot electroweak phase transition, Phys. Rev. Lett.82(1999) 21-24, [hep-ph/9809291]. [8] C. Caprini et al.,Detecting gravitational waves from cosmological phase transitions with LISA: an update,JCAP03(2020) 024, [1910.13125]. [9] M. Laine and A. Vuorinen,Basics of Thermal Field Theory, vol. 925. Springer, 2016,"},{"citing_arxiv_id":"2604.20768","ref_index":135,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Primordial Magnetogenesis and Gravitational Waves from ALP-assisted Phase Transition","primary_cat":"hep-ph","submitted_at":"2026-04-22T16:57:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"ALP-assisted first-order phase transitions can explain observed intergalactic magnetic fields and produce detectable gravitational waves, linking cosmology with particle physics searches.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"Conaci, L. Delle Rose, P.S.B. Dev and A. Ghoshal,Slaying axion-like particles via gravitational waves and primordial black holes from supercooled phase transition,JHEP12 (2024) 196 [2401.09411]. [134] C. Grojean and G. Servant,Gravitational Waves from Phase Transitions at the Electroweak Scale and Beyond,Phys. Rev. D75(2007) 043507 [hep-ph/0607107]. [135] T. Hambye and A. Strumia,Dynamical generation of the weak and Dark Matter scale,Phys. Rev. D88(2013) 055022 [1306.2329]. [136] S. Iso, P.D. Serpico and K. Shimada,QCD-Electroweak First-Order Phase Transition in a Supercooled Universe,Phys. Rev. Lett.119(2017) 141301 [1704.04955]. [137] M. Arteaga, A. Ghoshal and A. Strumia,Gravitational waves and black holes from the phase"},{"citing_arxiv_id":"2604.19197","ref_index":78,"ref_count":2,"confidence":0.9,"is_internal_anchor":true,"paper_title":"CP-violating multi-field phase transitions and gravitational waves in a hidden NJL sector","primary_cat":"hep-ph","submitted_at":"2026-04-21T08:07:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Multi-field tunneling analysis in a CP-violating NJL model yields a slow transition (β/H ~ 100) whose stochastic gravitational-wave signal is detectable by μAres and insensitive to the CP angle.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"adopt the percolation temperatureT ∗ =T p as the characteristic reference point. The inverse duration of the phase transition, normalized by the Hubble parameter, is evaluated as [3] β H∗ =T ∗ d dT \u0012 S3 T \u0013 T=T ∗ .(25) Similarly, the phase transition strengthα, which quantifies the latent heat released during the vacuum transition relative to the background radiation energy density, is defined as 8 [78, 79] α= 1 ρrad(T∗) \u0014 ∆V(σ, η, T)−T∆ \u0012 ∂Vef f(σ, η, T) ∂T \u0013\u0015 T=T ∗ ,(26) where ∆V=V f alse −V true. The radiation energy density is given byρ rad(T∗) =π 2g∗T 4 ∗ /30. Here,g ∗ denotes the effective number of relativistic degrees of freedom in the thermal plasma [80-82], which systematically incorporates contributions from both the Standard Model and the hidden sector atT ∗."},{"citing_arxiv_id":"2604.09081","ref_index":27,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Probing High-Quality Axions with Gravitational Waves","primary_cat":"hep-ph","submitted_at":"2026-04-10T08:09:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"High-quality axion models with N_DW=1 and dark matter abundance requirement restrict the gauge breaking scale to 1.6e11-1e16 GeV, yielding a band of gravitational wave signals from two-step phase transitions consistent with current observations.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"\u0012 β H \u0013−1 vw \u0012 κνα 1 +α \u00132 × \u0012 g∗ 100 \u0013−1/3\u0012 f fsw \u00133\u0012 7 4 + 3(f /fsw)2 \u00137/2 ,(12) The peak frequency is fsw = 1.9×10 −5 β H T 100 GeV 1 vw \u0010 g∗ 100 \u00111/6 Hz,(13) and the duration of the acoustic period is τsw = min \u0014 1 H , R∗ ¯Uf \u0015 ,(14) whereR ∗ =v w(8π)1/3/βis the mean bubble separation, U 2 f ≈3κ να/4(1 +α) is the root-mean-square fluid velocity [27, 35, 36],κ ν denotes the efficiency factor for the conversion of latent heat into kinetic energy of the fluidκ ν = √α/(0.135 + √0.98 +α) [37]. (II) Cosmic strings:The spontaneous breaking of the gaugedU(1) g symmetry leads to the formation of CSs [19]. The subsequent evolution of the string network is well described by the Nambu-Goto dynamics together"},{"citing_arxiv_id":"2603.09126","ref_index":120,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Dark matter in classically conformal theories: WIMP and supercooling","primary_cat":"hep-ph","submitted_at":"2026-03-10T02:57:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Classically conformal SU(2)_X model with triplet dark scalar yields viable WIMP and supercooled DM parameter spaces whose production histories are set by the model's first-order phase transition, with gravitational waves as a common probe.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.02458","ref_index":12,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Cosmic Collider Gravitational Waves sourced by Right-handed Neutrino production from Bubbles: Testing Seesaw, Leptogenesis and Dark Matter","primary_cat":"astro-ph.CO","submitted_at":"2026-01-05T18:57:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Bubble collisions in a seesaw model produce right-handed neutrinos that source novel gravitational waves detectable by LISA, ET, and LVK while allowing the lightest RHN to explain dark matter or enable leptogenesis.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":", JCAP04, 001 (2016), arXiv:1512.06239 [astro-ph.CO]. [9] C. Caprini and D. G. Figueroa, Class. Quant. Grav.35, 163001 (2018), arXiv:1801.04268 [astro-ph.CO]. [10] C. Capriniet al., JCAP03, 024 (2020), arXiv:1910.13125 [astro-ph.CO]. [11] P. Athron, C. Bal' azs, A. Fowlie, L. Morris, and L. Wu, Prog. Part. Nucl. Phys.135, 104094 (2024), arXiv:2305.02357 [hep-ph]. [12] A. Kosowsky, M. S. Turner, and R. Watkins, Phys. Rev. Lett.69, 2026 (1992). [13] C. Caprini, R. Durrer, and G. Servant, Phys. Rev. D77, 124015 (2008), arXiv:0711.2593 [astro-ph]. [14] S. J. Huber and T. Konstandin, JCAP09, 022 (2008), arXiv:0806.1828 [hep-ph]. [15] D. Bodeker and G. D. Moore, JCAP05, 009 (2009), arXiv:0903.4099 [hep-ph]. [16] R. Jinno and M."},{"citing_arxiv_id":"2511.21488","ref_index":23,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Bayesian analysis of the complex singlet model with phase transition gravitational waves","primary_cat":"hep-ph","submitted_at":"2025-11-26T15:21:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Bayesian forecasts for the Taiji detector constrain complex singlet model parameters through electroweak phase transition gravitational wave signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.02612","ref_index":68,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Model Parameter Reconstruction of Electroweak Phase Transition with TianQin and LISA: Insights from the Dimension-Six Model","primary_cat":"hep-ph","submitted_at":"2025-11-04T14:35:27+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations show TianQin and LISA can reconstruct the dimension-six model parameter Λ to sub-percent statistical precision for strong signals using Fisher, Bayesian sampling, and machine learning on data with noise and foregrounds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.00996","ref_index":23,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Measuring gravitational wave spectrum from electroweak phase transition and Higgs self-couplings","primary_cat":"hep-ph","submitted_at":"2025-11-02T16:07:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Frequency-domain simulations of the Taiji mission, including noise and foregrounds, demonstrate that the stochastic gravitational wave background from an electroweak phase transition can constrain Higgs cubic and quartic self-couplings in a singlet-extended Standard Model despite degeneracies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.19009","ref_index":102,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Finite-temperature Yang-Mills theories with the density of states method: towards the continuum limit","primary_cat":"hep-lat","submitted_at":"2025-09-23T13:51:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Density-of-states lattice study of the first-order phase transition in Sp(4) Yang-Mills theory at finite temperature, confirming metastability and surface tension for two temporal extents toward the continuum limit.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":",Science with the space-based interferometer eLISA. II: Gravitational waves from cosmological phase transitions,JCAP04(2016) 001 [1512.06239]. [100]LISAcollaboration,Laser Interferometer Space Antenna,1702.00786. [101]LIGO Scientificcollaboration,Exploring the Sensitivity of Next Generation Gravitational Wave Detectors,Class. Quant. Grav.34(2017) 044001 [1607.08697]. [102] S. Isoyama, H. Nakano and T. Nakamura,Multiband Gravitational-Wave Astronomy: Observing binary inspirals with a decihertz detector, B-DECIGO,PTEP 2018(2018) 073E01 [1802.06977]. [103] J. Baker et al.,The Laser Interferometer Space Antenna: Unveiling the Millihertz Gravitational Wave Sky, 7, 2019. [104] V. Brdar, A.J. Helmboldt and J. Kubo,Gravitational"},{"citing_arxiv_id":"2509.10456","ref_index":68,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Gravitational Wave Signature and the Nature of Neutrino Masses: Majorana, Dirac, or Pseudo-Dirac?","primary_cat":"hep-ph","submitted_at":"2025-09-12T17:59:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"In the minimal B-L gauge extension, Majorana neutrinos at high breaking scale produce flat GW spectra from cosmic strings, Dirac at low scale produce peaked spectra from first-order phase transitions, and pseudo-Dirac produce kink features from domain wall annihilation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.08011","ref_index":57,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Primordial black holes and magnetic fields in conformal neutrino mass models","primary_cat":"hep-ph","submitted_at":"2025-05-12T19:24:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Conformal U(1)' seesaw models produce PBHs contributing to dark matter and helical magnetic fields at seesaw scales of 10^4-10^11 GeV, with observable GW, microlensing, and Hawking signals at LISA, Roman, and future gamma-ray telescopes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2504.03837","ref_index":77,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Exploring Leptogenesis in the Era of First Order Electroweak Phase Transition","primary_cat":"hep-ph","submitted_at":"2025-04-04T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Low-scale leptogenesis becomes viable in the neutrino seesaw framework when a first-order electroweak phase transition allows sphalerons to convert lepton asymmetry into baryon asymmetry at temperatures below the Standard Model decoupling point.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2503.01962","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Curvature Perturbations from First-Order Phase Transitions: Implications to Black Holes and Gravitational Waves","primary_cat":"hep-ph","submitted_at":"2025-03-03T19:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Covariant analysis of curvature perturbations from first-order phase transitions reveals gauge-dependent overestimation of primordial black holes and gravitational waves in prior non-covariant calculations, leading to strong suppression of both signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2408.03649","ref_index":97,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Probing radiative electroweak symmetry breaking with colliders and gravitational waves","primary_cat":"hep-ph","submitted_at":"2024-08-07T09:24:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Radiative electroweak symmetry breaking with a logarithmic potential yields analytical vacuum solutions, four thermal history patterns, and supercooled FOPT gravitational waves whose signals combined with collider data can probe conformal scales to 10^5-10^8 GeV.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2404.19197","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Does the Electron EDM Preclude Electroweak Baryogenesis ?","primary_cat":"hep-ph","submitted_at":"2024-04-30T01:49:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"First-order gradient CP-violating sources in EWBG quantum transport relax electron EDM bounds and increase viability compared to prior approximations in a model illustration.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2002.04615","ref_index":25,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"New Sensitivity Curves for Gravitational-Wave Signals from Cosmological Phase Transitions","primary_cat":"hep-ph","submitted_at":"2020-02-11T19:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Defines peak-integrated sensitivity curves (PISCs) that fold in the expected spectral shape of gravitational waves from cosmological phase transitions and supplies semianalytical fits plus public data for major detectors.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"standard references on this subject. For more recent work on the dynamics of cosmological phase transitions and the shape of the resulting GW signal, we refer to Refs. [139-155]. - 5 - We begin by pointing out that, among Refs. [24, 25], only Ref. [24] presents semiana- lytical expressions for all three GW sources, Ω b, Ω s, and Ω t. The discussion in Ref. [25] is more conservative in the sense that it solely accounts for the signal from sound waves, which is in many cases much stronger than the signal from bubble collisions and in general much better understood from a theoretical perspective than the signal from turbulence. Ref. [25] also distinguishes between two different expressions for Ω s, depending on whether the time"}],"limit":50,"offset":0}