{"total":12,"items":[{"citing_arxiv_id":"2606.28554","ref_index":269,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The NANOGrav 15 yr Data Set: Impacts of Customized Chromatic Noise Models on Gravitational Wave Analyses","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T19:14:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Customized chromatic noise models applied to NANOGrav 15 yr data raise the Bayes factor for Hellings-Downs GWB correlations by a factor of ~8, lower the amplitude to 2.1e-15, and increase the spectral index to 3.5.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05320","ref_index":54,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational Wave Imprints of a High-Quality Axion and the Origin of Flavor Hierarchies","primary_cat":"hep-ph","submitted_at":"2026-06-03T18:07:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Gauged U(1)_F flavor symmetries shield the axion from quantum gravity corrections, yielding unit domain wall number and a plateau-valley GW spectrum from flavonic and axionic strings as a probe of flavored axion dark matter.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02706","ref_index":142,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Majoron Dark Matter, High-Scale Seesaw, and Leptogenesis","primary_cat":"hep-ph","submitted_at":"2026-06-01T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Majoron dark matter is viable for sub-MeV masses in high-scale seesaw models with thermal leptogenesis, produced via misalignment and cosmic strings in pre- and post-inflationary scenarios and constrained by CMB, X-ray, and gravitational wave observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.31600","ref_index":99,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational Waves from hybrid defects as probe of Flavor symmetry breaking: Machine-Learning Approach","primary_cat":"astro-ph.CO","submitted_at":"2026-05-29T17:59:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Hybrid string-bounded domain wall networks from sequential U(1)_F and Z2 symmetry breaking generate a GW spectrum with a unique low-frequency slope that future detectors can observe and an MLP surrogate can characterize for fast SNR inference.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.28097","ref_index":74,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"New gravitational-wave templates for metastable cosmic strings: Loop breaking versus network collapse","primary_cat":"hep-ph","submitted_at":"2026-04-30T16:40:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Metastable cosmic strings produce a gravitational wave background that is best modeled with three parameters (string tension Gμ plus independent time scales t_LB and t_NC), yielding a compact analytical spectrum when t_LB greatly exceeds t_NC.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"production,\"Phys. Rev. D83(2011) 083514, arXiv:1101.5173 [astro-ph.CO]. [72] A. Monin and M. B. Voloshin, \"The Spontaneous breaking of a metastable string,\"Phys. Rev. D78(2008) 065048, arXiv:0808.1693 [hep-th]. [73] L. Tranchedone, E. Carragher, E. Hardy, and N. K. van IJcken, \"Metastable cosmic strings are broken at the start,\" arXiv:2601.04320 [hep-ph]. [74] G. Lazarides, R. Maji, and Q. Shafi, \"Gravitational waves from quasi-stable strings,\"JCAP08no. 08, (2022) 042, arXiv:2203.11204 [hep-ph]. [75] G. Lazarides, R. Maji, and Q. Shafi, \"Superheavy quasistable strings and walls bounded by strings in the light of NANOGrav 15 year data,\"Phys. Rev. D108no. 9, (2023) 095041,arXiv:2306.17788 [hep-ph]. [76] R."},{"citing_arxiv_id":"2604.21642","ref_index":36,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Exploring the statistical anisotropy of primordial curvature perturbations with pulsar timing arrays","primary_cat":"gr-qc","submitted_at":"2026-04-23T12:57:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A phenomenological dipole anisotropy in primordial perturbations induces dipolar and quadrupolar anisotropies in SIGW energy density spectra, producing frequency-dependent PTA overlap reduction functions that depend on pulsar sky distribution, but NANOGrav 15-year data yields no significant evidence","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[31] J.-P. Li, S. Wang, Z.-C. Zhao, and K. Kohri, JCAP05, 109 (2024), arXiv:2403.00238 [astro-ph.CO]. [32] A. Vilenkin, Phys. Lett. B107, 47 (1981). [33] C. J. Hogan and M. J. Rees, Nature311, 109 (1984). [34] T. Vachaspati and A. Vilenkin, Phys. Rev. D31, 3052 (1985). [35] T. Damour and A. Vilenkin, Phys. Rev. D71, 063510 (2005), arXiv:hep-th/0410222. [36] J. J. Blanco-Pillado and K. D. Olum, Phys. Rev. D96, 104046 (2017), arXiv:1709.02693 [astro-ph.CO]. [37] C. Ringeval and T. Suyama, JCAP12, 027 (2017), arXiv:1709.03845 [astro-ph.CO]. [38] J. Baeza-Ballesteros, E. J. Copeland, D. G. Figueroa, and J. Lizarraga, Phys. Rev. D110, 043522 (2024), arXiv:2308.08456 [astro-ph.CO]. [39] B. Fu, A. Ghoshal, and S."},{"citing_arxiv_id":"2604.09081","ref_index":40,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"The subsequent evolution of the string network is well described by the Nambu-Goto dynamics together with string intercommutation, resulting in a scaling net- work composed of long strings and loops [38-40]. The loops gradually lose energy through gravitational radia- tion, giving rise to a SGWB. The present-day GW spectrum from string loops can be expressed as [40, 41] ΩCS GW(lnf)h2 = 8πΓG2µ2f h2 3H2 0 ζ 4 3 ,∞ \u0001 ∞X j=1 j−4/3 2j f2 × Z ∞ 0 dz H(z)(1 +z) 6 n \u0012 t(z), 2j (1 +z)f \u0013 ,(15) whereGµ∼Gπf 2 g denotes the dimensionless string tension [42], Γ≃50 is the loop emission efficiency [40, 41, 43-45], andζ 4 3 ,∞ \u0001 =P∞ j=1 j−4/3 arises from the cusp-dominated GW emission spectrum. HereH(z) andt(z) are the Hubble parameter and cosmic time, re-"},{"citing_arxiv_id":"2604.08142","ref_index":22,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Caustic formation in DBI models: Wave propagation on planar domain walls","primary_cat":"hep-th","submitted_at":"2026-04-09T12:01:28+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":"09(2024), 047; [arXiv:2406.17053 [astro-ph.CO]]. [19] T. W. B. Kibble,Topology of Cosmic Domains and Strings, J. Phys. A9(1976), 1387- 1398. [20] T. Vachaspati and A. Vilenkin,Gravitational Radiation from Cosmic Strings, Phys. Rev. D31(1985), 3052. [21] A. Vilenkin and T. Vachaspati,Radiation of Goldstone Bosons From Cosmic Strings, Phys. Rev. D35(1987), 1138. [22] J. J. Blanco-Pillado and K. D. Olum,Stochastic gravitational wave background from smoothed cosmic string loops, Phys. Rev. D96(2017) no.10, 104046; [arXiv:1709.02693 [astro-ph.CO]]. [23] J. Baeza-Ballesteros, E. J. Copeland, D. G. Figueroa and J. Lizarraga,Particle and gravitational wave emission by local string loops: Lattice calculation, Phys. Rev."},{"citing_arxiv_id":"2509.14323","ref_index":88,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"High-Quality Axion Dark Matter at Gravitational Wave Interferometers","primary_cat":"hep-ph","submitted_at":"2025-09-17T18:00:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"In gauged U(1) completions enabling high-quality axion dark matter, cosmic string loops generate a stochastic gravitational wave background with an infrared break frequency that exceeds foregrounds above 10^14 GeV breaking scales and offers a probe at interferometers.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"background [82], while the remaining parameter space can be probed by future GW interferometers such as CE [83, 84] and ET [85], as discussed in the following sections. In this class of models [23, 39], gauge CS form at a temperature scaleT∼f g, while global CS form around T∼f a [23, 81]. The gauge strings predominantly radiate gravitational waves [88], whereas global strings primarily loseenergythroughGoldstonebosonemission[89]. Akey feature of axion models is the formation of DW when the temperature-dependent axion mass becomes comparable to the Hubble parameterH, and the axion field begins to rolltowardtheminimumofitspotential[7,8]. Theevolu- tion and fate of the resulting string-wall network are gov-"},{"citing_arxiv_id":"2509.10456","ref_index":42,"ref_count":1,"confidence":0.98,"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":"2311.01300","ref_index":263,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Waveform Modelling for the Laser Interferometer Space Antenna","primary_cat":"gr-qc","submitted_at":"2023-11-02T15:15:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review of existing waveform models for LISA sources and the challenges that must still be overcome.","context_count":1,"top_context_role":"background","top_context_polarity":"support","context_text":"More stringent bounds on tension generally invoke additional assumptions [320]. Gravitational wave experiments [252, 274, 303, 321] can monitor the occurrence of bursts. In particular, the LVK set a bound GµS/c2 ≲ 4 × 10−15 based on non-detection of assumed cusp-like bursts [322]. Long-term pulsar timing searches for a stochastic background have set the bound of GµS/c2 ≲ 1.5 × 10−11 [263, 265, 266, 308]. In the future LISA may achieve limits as low as GµS ∼ 10−17 for Nambu-Goto strings [275, 323]. 2.6.3. Loop sources for LISA The VOS model for the minimally coupled string network generates a loop size distribution weighted towards small sizes [264]. For string tensions GµS/c2 ≪ 10−7 the string loops are the most important elements of the network for"},{"citing_arxiv_id":"2003.01100","ref_index":242,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The landscape of QCD axion models","primary_cat":"hep-ph","submitted_at":"2020-03-02T18:51:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Review classifies QCD axion models extending the standard mass-coupling window and updates bounds from cosmology, astrophysics, and experiments.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"on a timescale comparable to the Hubble time, and describes a power spectrum ranging over all modes from k≈ 1/ℓ(tI)≈ H(tI)/αloop to infinity [202, 230]. On the other hand, assuming that strings efficiently shrink emitting all of their energy at once leads to a flat power spectrum per logarithmic interval with an infrared cutoff at the wave modek≈ H and an ultraviolet cutoff atk = fa, with a harder spectral index q = 1 [199, 241, 242]. Demanding that the spectrum is normalised over the given interval results in F (k) =    q−1 αq−1 loop (k H )−q , for q > 1 , 1 ln(fa/H) H k , for q = 1 . (183) The integration of Eq. (182) with the spectrum in Eq. (183) andq > 1 finally leads to nstr a ≈ (1− 3wstr) πf 2 a 2tosc × { αloop q−1 q ln (fatosc) , for q > 1 , 1, for q = 1 . (184) This expression shows that most of the axions are radiated by loops right beforetosc, when DWs dissipate"}],"limit":50,"offset":0}