{"total":27,"items":[{"citing_arxiv_id":"2607.00072","ref_index":12,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Precision Solar System Dynamics for Ultralight Dark Matter Search","primary_cat":"hep-ph","submitted_at":"2026-06-30T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Current interplanetary range measurements could probe ultralight dark matter at masses around 10^{-15} eV if its solar system density were 10^5 times the local value.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.31476","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Landau-Zener formula and resonant axion conversion in neutron star magnetospheres","primary_cat":"hep-ph","submitted_at":"2026-06-30T10:51:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The Landau-Zener approximation for axion-photon conversion in neutron star magnetospheres fails when resonance width exceeds conversion region size, leading to revised axion constraints from optical-band searches.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.30739","ref_index":53,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Fuzzy Dark Matter Halo Mass Functions at Cosmic Dawn","primary_cat":"astro-ph.CO","submitted_at":"2026-06-29T18:00:06+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"New simulation-based fitting formula for FDM halo mass functions at z=6-11, with ~30% weaker suppression than earlier formulas for m c²=10^{-21} eV at M~3e9 solar masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28488","ref_index":84,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Dark energy from neutrino interactions in Unimodular Gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Neutrino interactions in unimodular gravity produce dynamical dark energy whose evolution fits late-time cosmological data for interaction strengths around 10^12 eV^{-2} at 2 sigma for sub-meV neutrino masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20524","ref_index":32,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"String Axiverse Enhancement of Superradiant Dark Matter Production","primary_cat":"hep-ph","submitted_at":"2026-06-18T17:38:19+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17176","ref_index":42,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Tracing Ultra Light Axions in Post-reionization, Lyman-$\\alpha$ and CMB Missions","primary_cat":"astro-ph.CO","submitted_at":"2026-06-15T18:15:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Fisher forecasts indicate joint post-reionization LSS cross-spectra and CMB-S4-like data can reach O(10^{-4}) uncertainty on ultra-light axion fraction for m_a ≲ 10^{-28} eV, with peak sensitivity near 10^{-25} eV.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.07749","ref_index":199,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Flavor phenomenology of light dark particles","primary_cat":"hep-ph","submitted_at":"2026-06-05T18:00:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Review surveying limits and prospects for flavor-violating decays of light axion-like particles, highlighting complementarity of lab, astro, and cosmo probes up to 10^12 GeV scales.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"particular due to IR divergences which worsen the convergence of perturba- tive QCD calculations. For flavor-violating vertices parts of these corrections have been calculated in Ref. [196], but it is questionable to what degree the gluon can be treated as a weakly coupled degree of freedom wheng s ≳1, so perturbation theory can only be trusted atT≫TeV [199]. Neverthe- less one may expect that production rates based solely on flavor-violating 78 decays are a reasonably good approximation of the full calculation, so the result for the quarks sector in Ref. [196] should be valid. Still a complete analysis of next-to-leading-order (NLO) corrections in this case is desirable, in particular for cosmological limits, as discussed in Section 4."},{"citing_arxiv_id":"2606.06484","ref_index":11,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Phenomenology of Inflaton-Driven Early QCD Confinement and Solution to Axion Isocurvature Problem","primary_cat":"astro-ph.CO","submitted_at":"2026-06-04T17:58:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Inflaton-gluon coupling induces early QCD confinement to suppress axion isocurvature perturbations and enable axion dark matter production in alpha-attractor inflation models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02706","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"on the majoron,Phys. Lett. B299(1993) 90 [hep-ph/9209285]. [14] J.M. Cline, K. Kainulainen and K.A. Olive,Constraints on majoron models, neutrino masses and baryogenesis,Astropart. Phys.1(1993) 387 [hep-ph/9304229]. [15] I.Z. Rothstein, K.S. Babu and D. Seckel,Planck scale symmetry breaking and majoron physics,Nucl. Phys. B403(1993) 725 [hep-ph/9301213]. [16] V. Berezinsky and J.W.F. Valle,The KeV majoron as a dark matter particle,Phys. Lett. B 318(1993) 360 [hep-ph/9309214]. [17] D. Kazanas, R.N. Mohapatra, S. Nasri and V.L. Teplitz,Neutrino mass, dark matter and inflation,Phys. Rev. D70(2004) 033015 [hep-ph/0403291]. [18] S.M. Boucenna, S. Morisi, Q. Shafi and J.W.F. Valle,Inflation and majoron dark matter in"},{"citing_arxiv_id":"2605.21092","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Audible Axion Magnetogenesis: Linking Intergalactic Magnetic Fields and Gravitational Waves","primary_cat":"hep-ph","submitted_at":"2026-05-20T12:24:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Axion-like particles in the trapped misalignment mechanism produce observable gravitational waves while generating intergalactic magnetic fields that exceed blazar lower bounds in the parameter space promising for gravitational wave detection.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Axions [1-4] and axion-like particles (ALPs) are among the most compelling dark matter candidates [5-7], may provide a framework for realizing cosmic inflation [8-13], and naturally arise in many ultraviolet completions of the Standard Model (SM) [14-17]. Unfortunately, the regime of large decay constants fϕ, where the ALP be- comes effectively invisible, remains challenging to probe experimentally [18]. In the audible axion model, an oscil- lating ALP triggers a tachyonic resonance in the equation of motion of an Abelian gauge boson, leading to copious production of gauge quanta in the early Universe [19-37]; see also [38-56]. This induces large anisotropies in the cosmic fluid, resulting in the production of a stochastic gravitational wave (GW) background and thereby open-"},{"citing_arxiv_id":"2605.17211","ref_index":41,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constraints on Self-Interacting Fuzzy Dark Matter from the Stellar Kinematics of the Dwarf Galaxy Leo II","primary_cat":"astro-ph.CO","submitted_at":"2026-05-17T01:00:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Using Jeans analysis of Leo II stellar kinematics, the paper constrains the fuzzy dark matter mass m_a and self-interaction parameter f_a, finding 95% CL lower limits on m_a in the (1-10)×10^{-22} eV range for |f_a^{-1}| ≲ 10^{-14} GeV^{-1}.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17178","ref_index":32,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"An EFT Map of Axion Dark Radiation from Reheating","primary_cat":"hep-ph","submitted_at":"2026-05-16T22:29:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"An EFT with inflaton-dependent axion kinetic term organizes direct decay and annihilation production during reheating, yielding ΔN_eff contributions that scale as T_rh^{-2} and T_rh^{4/3} respectively and allowing a two-dimensional map of constraints on Wilson coefficients and reheating temperature.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15261","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Magnetic Turbulence Boosts Supernova Signals of Axion-Photon Conversion","primary_cat":"hep-ph","submitted_at":"2026-05-14T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Turbulent magnetic fields enhance axion-photon conversion signals from supernovae, improving limits on axion-proton and axion-photon couplings by up to two orders of magnitude.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15192","ref_index":6,"ref_count":3,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Isocurvature-Free QCD Axion Dark Matter from Inflaton-Driven Early QCD: the Necessity of Inflationary Plateaus","primary_cat":"astro-ph.CO","submitted_at":"2026-05-14T17:59:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Inflaton-gluon coupling during inflation requires p=2 plateau models to produce isocurvature-free QCD axion dark matter.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11078","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"An ultra-broadband axion dark matter experiment","primary_cat":"hep-ph","submitted_at":"2026-05-11T18:00:03+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A dc SQUID operated at the flux sweet spot with lock-in modulation yields an ultra-broadband axion search with projected sensitivity |g_aγγ| ≳ 10^{-16} GeV^{-1} across 15 orders of magnitude in mass.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"59, 247-289 (2021), arXiv:2101.11735 [astro- ph.CO]. [16] Igor G. Irastorza and Javier Redondo, \"New experimental approaches in the search for axion-like particles,\" Prog. Part. Nucl. Phys.102, 89-159 (2018), arXiv:1801.08127 [hep-ph]. [17] Ciaran A. J. O'Hare, \"Cosmology of axion dark matter,\" PoSCOSMICWISPers, 040 (2024), arXiv:2403.17697 [hep-ph]. [18] Andrea Caputo and Georg Raffelt, \"Astrophysical Axion Bounds: The 2024 Edition,\" PoSCOSMICWISPers, 041 (2024), arXiv:2401.13728 [hep-ph]. [19] P. Sikivie and Q. Yang, \"Bose-Einstein Condensation of Dark Matter Axions,\" Phys. Rev. Lett.103, 111301 (2009), arXiv:0901.1106 [hep-ph]. [20] Alan H. Guth, Mark P. Hertzberg, and C. Prescod- Weinstein, \"Do Dark Matter Axions Form a Condensate"},{"citing_arxiv_id":"2605.00648","ref_index":23,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Anisotropy of Cosmic Background Photons from Annihilating/Decaying Dark Matter","primary_cat":"hep-ph","submitted_at":"2026-05-01T13:29:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A comprehensive formulation is given for the angular power spectrum of photons from dark matter annihilation or decay, stressing that detector energy resolution is essential for accurate evaluation of line photon signals.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"1We are interested in the case that the dark matter lifetime is much longer than the present age of the universe (t0). Thus we take the factore −Γt0 to be unity. We also neglect the attenuation of the photon when traveling the cosmological distance [21, 22]. It is justified for the photon energy range that we will be interested in. 3 whereN γ is the number of photon produced per decay. A typical example ofN γ = 2 is axion-like particles [23], whileN γ = 1 is sterile neutrino [24]. In Refs. [17, 18], an axion- like particle decaying into photon plus dark photon has been considered, which is another example ofN γ = 1. By substituting (2.6), we obtain I(ω) = Z dω′ (ω′)q−1 P(ω ′) 1 8π ρDM,0 m NγΓ H(z) 1+z= m 2ω′ .(2.7) Forq= 1, the mean flux Ihas a unit of, e.g., [cm −2s−1sr−1], while forq= 2 it has a unit of,"},{"citing_arxiv_id":"2604.28062","ref_index":14,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Semi-analytic bounds on axion-like-particle supernovae emission","primary_cat":"hep-ph","submitted_at":"2026-04-30T16:08:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Semi-analytic modeling of supernova cooling with six PNS parameters yields bounds on axion-nucleon coupling versus ALP mass that match numerical simulation results.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"(2020), arXiv:1910.02080 [hep-ph]. [10] P. Bittar, G. Burdman, and G. M. Salla, Phys. Rev. D 112, 055039 (2025), arXiv:2410.00964 [hep-ph]. [11] F. Wilczek, Phys. Rev. Lett.49, 1549 (1982). [12] P. Sikivie, Phys. Rev. Lett.51, 1415 (1983). [13] L. Di Luzio, M. Giannotti, E. Nardi, and L. Visinelli, Phys. Rept.870, 1 (2020), arXiv:2003.01100 [hep-ph]. [14] C. A. J. O'Hare, PoSCOSMICWISPers, 040 (2024), arXiv:2403.17697 [hep-ph]. [15] A. Bharucha, F. Br¨ ummer, N. Desai, and S. Mutzel, JHEP02, 141 (2023), arXiv:2209.03932 [hep-ph]. [16] G. Armando, P. Panci, J. Weiss, and R. Ziegler, Phys. Rev. D109, 055029 (2024), arXiv:2310.05827 [hep-ph]. [17] W. Beenakker, D. Mikkers, A. V. Phan, and S. Westhoff,"},{"citing_arxiv_id":"2604.14285","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cornering MeV-GeV Axions and Dark Photons with LDMX","primary_cat":"hep-ph","submitted_at":"2026-04-15T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"LDMX can close much of the sub-100 MeV blind spot for axions and dark photons via charged track and momentum reconstruction.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Department of Energy, Office of Science, Office of High Energy Physics; by the National Science Foundation un- der Grant No. PHY-2310429; by the Simons Foundation through Investigator Award No. 824870; and by the John Templeton Foundation under Award No. 63595. 9 ∗ arusso00@stanford.edu [1] S. Goriet al., Dark Sector Physics at High-Intensity Ex- periments (2022), arXiv:2209.04671 [hep-ph]. [2] C. A. J. O'Hare, PoSCOSMICWISPers, 040 (2024), arXiv:2403.17697 [hep-ph]. [3] N. Blinov, N. Craig, M. J. Dolan, J. de Vries, P. Draper, I. G. Garcia, B. Lillard, and J. Shelton, inSnowmass 2021(2022) arXiv:2203.07218 [hep-ph]. [4] M. Cirelli, A. Strumia, and J. Zupan, SciPost Phys. Rev. , 1 (2026). [5] B. Batell, N. Blinov, C. Hearty, and R. McGehee, in"},{"citing_arxiv_id":"2604.13181","ref_index":21,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Searching for axions with quantum interferometry","primary_cat":"hep-ph","submitted_at":"2026-04-14T18:03:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Axion-photon coupling imprints measurable Aharonov-Bohm and Berry phases in superconducting circuits and interferometers, projecting sensitivity to g_aγγ ~ 7.8e-14 GeV^{-1} at m_a ~ 1e-10 eV.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"search for dark matter,\"Nature562no. 7725, (2018) 51-56,arXiv:1810.01668 [astro-ph.CO]. 17 [19] F. Chadha-Day, J. Ellis, and D. J. E. Marsh, \"Axion dark matter: What is it and why now?,\"Sci. Adv.8 no. 8, (2022) abj3618,arXiv:2105.01406 [hep-ph]. [20] C. A. J. O'Hare, \"Cosmology of axion dark matter,\" PoSCOSMICWISPers(2024) 040, arXiv:2403.17697 [hep-ph]. [21] S. J. Asztalos, G. Carosi, C. Hagmann, D. Kinion, K. van Bibber, M. Hotz, L. J. Rosenberg, G. Rybka, J. Hoskins, J. Hwang, P. Sikivie, D. B. Tanner, R. Bradley, J. Clarke, and ADMX Collaboration, \"SQUID-Based Microwave Cavity Search for Dark-Matter Axions,\"Phys. Rev. Lett.104no. 4, (Jan., 2010) 041301,arXiv:0910.5914 [astro-ph.CO]. [22]ADMXCollaboration, N."},{"citing_arxiv_id":"2603.10189","ref_index":21,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Searching for axions with time resolved pulsar polarimetry","primary_cat":"hep-ph","submitted_at":"2026-03-10T19:32:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Time-resolved optical polarimetry of the Crab pulsar is used to place bounds on the axion-photon coupling via oscillating axion fields induced by the pulsar's magnetic field.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.13815","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Stripped-Envelope Supernovae for QCD Axion Detection","primary_cat":"hep-ph","submitted_at":"2025-11-17T19:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Stripped-envelope supernovae enable QCD axion detection to masses around 10^{-4} eV via gamma-ray signals from conversion in progenitor magnetic fields.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.10617","ref_index":10,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Dark Matter from Holography","primary_cat":"astro-ph.CO","submitted_at":"2025-11-13T18:45:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Holographic dark matter arises from the Ricci cutoff in a baryon-plus-radiation universe, matching observed densities and reversing the sign of pre-existing negative vacuum energy to match observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.22592","ref_index":25,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing Axion-Photon conversion via circular polarization imprints in the CMB $V$-mode observations","primary_cat":"astro-ph.CO","submitted_at":"2025-10-26T09:20:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Proposes that axion-photon conversion in pre-CMB helical magnetic fields imprints detectable V-mode polarization in the CMB, allowing CLASS 40 GHz observations to constrain ALP masses 10^{-10} to 10^{-8} eV and their photon coupling under optimistic nG field assumptions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.17977","ref_index":10,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Growth of Structure in Multi-species Wave Dark Matter","primary_cat":"astro-ph.CO","submitted_at":"2025-10-20T18:00:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Derives the power spectrum evolution and cross-spectra for arbitrary multi-species wave and particle dark matter, incorporating free-streaming, Jeans scales, and intrinsic fluctuations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.10708","ref_index":17,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Multimodal axion emissions from Abelian-Higgs cosmic strings","primary_cat":"hep-ph","submitted_at":"2025-10-12T17:16:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Lattice simulations of Abelian-Higgs cosmic strings with axion-gauge coupling show multimodal axion production that can account for GeV-scale dark matter while predicting observable dark radiation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.12722","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Completing Axion Double Level Crossings","primary_cat":"hep-ph","submitted_at":"2025-08-18T08:45:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Double level crossings are common in multi-axion mass mixing of Z_N axions and ALPs, occurring multiple times for large N in the light axion case but prevented by excessively large or small N in light and heavy scenarios respectively.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2506.12131","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Early Growth of Structure in Warm Wave Dark Matter","primary_cat":"astro-ph.CO","submitted_at":"2025-06-13T18:00:01+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Derives suppression of adiabatic perturbations and scale-dependent growth of isocurvature power in warm wave dark matter, verifies with Schrödinger-Poisson simulations, and proposes an analytic halo mass function.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}