{"total":13,"items":[{"citing_arxiv_id":"2606.31571","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nonlinear growth and amplification of phase-transition gravitational waves induced by cosmic expansion","primary_cat":"hep-ph","submitted_at":"2026-06-30T12:29:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"3D simulations in an expanding background show cosmic expansion drives nonlinear growth that amplifies gravitational-wave spectra from slow phase transitions by factors of 10 to 100.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09482","ref_index":42,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Primordial Black Holes from Slow Phase Transitions with Delayed Reheating: A Peak-Theory Approach","primary_cat":"hep-ph","submitted_at":"2026-06-08T13:39:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"PBH production from slow phase transitions with delayed reheating is modeled via peak theory and Monte Carlo simulations, showing extreme sensitivity to reheating efficiency and potential to explain all dark matter.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15197","ref_index":296,"ref_count":1,"confidence":0.98,"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":"09642 [hep-ph]. 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Saha, JCAP10, 053 (2023), arXiv:2307.00656 [hep-ph]. 37"},{"citing_arxiv_id":"2604.19197","ref_index":88,"ref_count":2,"confidence":0.98,"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":"Phys. Commun.256, 107480 (2020), 2002.00881. [84] Y. Chen, M. Huang, and Q.-S. Yan, JHEP05, 178 (2018), 1712.03470. [85] A. Kosowsky and M. S. Turner, Phys. Rev. D47, 4372 (1993), astro-ph/9211004. [86] R. Jinno and M. Takimoto, Phys. Rev. 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Zhang, Chin. Phys. C 45, 113104 (2021), 1907.13589. [61] J. Ellis, M. Lewicki, J. M. No, and V . Vaskonen, JCAP06, 024 (2019), 1903.09642. [62] J. Ellis, M. Lewicki, and V . Vaskonen, JCAP 11, 020 (2020), 2007.15586. [63] S. Jung and K. Kawana, PTEP 2022, 033B11 (2022), 2105.01217. [64] K. Kawana, Phys. Rev. D 105, 103515 (2022), 2201.00560. [65] Z. Zhao, Y . Di, L. Bian, and R.-G. Cai, JHEP 10, 158 (2023), 2204.04427. [66] L. Sagunski, P. Schicho, and D. Schmitt, Phys. Rev. D 107, 123512 (2023), 2303.02450. [67] A. Ahriche, S. Kanemura, and M. Tanaka, JHEP 01, 201 (2024), 2308.12676. [68] P. H. Ghorbani (2024), 2408.16475. [69] J. Braun and H. Gies, JHEP 06, 024 (2006), hep-ph/0602226. [70] R."},{"citing_arxiv_id":"2002.04615","ref_index":148,"ref_count":1,"confidence":0.98,"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":"While some authors estimate ϵ to be quite small, ϵ≃ 0.05··· 0.10 (see, e.g., Refs. [24, 47, 64]), based on the results presented in Ref. [132], other authors use values as large as ϵ = 1 (see, e.g. Ref. [159]). In our analysis, we will set ϵ = 0.10. For a more detailed discussion on the efficiency factors κs and κt, see also the recent analysis in Ref. [148]. In order to estimate the efficiency factors κb and κkin, one has to distinguish between three different types of phase transitions: (i) nonrunaway phase transitions in a plasma (NP), (ii) runaway phase transitions in a plasma (RP), and (iii) runaway phase transitions in vacuum (RV). In the first case, the bubble wall velocity saturates at a subluminal value,"},{"citing_arxiv_id":"1910.13125","ref_index":41,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Detecting gravitational waves from cosmological phase transitions with LISA: an update","primary_cat":"astro-ph.CO","submitted_at":"2019-10-29T07:58:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Updated LISA detection prospects for gravitational waves from phase transitions are derived from state-of-the-art sound-wave simulations, with a new web tool PTPlot provided for parameter scans.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"4 TeV, typically corresponding to several orders of magnitude of supercooling. Below this bound, the bubble wall approaches a steady state and a finite but highly relativistic bubble wall velocity. The latent heat is then transformed mostly into bulk motion. We will assume this is the case in our analysis, in contrast with our previous study [8] (see also [41] for an extended analysis of the issue). Notice that the PT strength parameter α scales as α∼ (∆m/Tn)4→∞ , while the fraction of energy in bulk motionK∼γ2 f (Tn/∆m)4 approaches unity [13]. Hence, the Lorentz factor of the fluid motion is of order γf∼ (∆m/Tn)2. This challenging regime is so far unexplored by hydrodynamic simulations and deserves further attention."}],"limit":50,"offset":0}